White dwarf

A white dwarf is a stellar core remnant composed mostly of electron-degenerate matter. A white dwarf is very dense: in an Earth sized volume, it packs a mass that is comparable to the Sun. No nuclear fusion takes place in a white dwarf; what light it radiates is from its residual heat.^[1] The nearest known white dwarf is Sirius B, at 8.6 light years, the smaller component of the Sirius binary star. There are currently thought to be eight white dwarfs among the hundred star systems nearest the Sun.^[2] The unusual faintness of white dwarfs was first recognized in 1910.^[3]^: 1 The name white dwarf was coined by Willem Jacob Luyten in 1922.

Thumb — Image of Sirius A and Sirius B taken by the Hubble Space Telescope. Sirius B, which is a white dwarf, can be seen as a faint point of light to the lower left of the much brighter Sirius A.

White dwarfs are thought to be the final evolutionary state of stars whose mass is not high enough to become a neutron star or black hole. This includes over 97% of the stars in the Milky Way.^[4]^: §1 After the hydrogen-fusing period of a main-sequence star of low or intermediate mass ends, such a star will expand to a red giant and fuse helium to carbon and oxygen in its core by the triple-alpha process. If a red giant has insufficient mass to generate the core temperatures required to fuse carbon (around 10⁹ K), an inert mass of carbon and oxygen will build up at its center. After such a star sheds its outer layers and forms a planetary nebula, it will leave behind a core, which is the remnant white dwarf.^[5] Usually, white dwarfs are composed of carbon and oxygen (CO white dwarf). If the mass of the progenitor is between 7 and 9 solar masses (M_☉), the core temperature will be sufficient to fuse carbon but not neon, in which case an oxygen–neon–magnesium (ONeMg or ONe) white dwarf may form.^[6] Stars of very low mass will be unable to fuse helium; hence, a helium white dwarf^[7]^[8] may form by mass loss in an interacting binary star system.^[9]

Because the material in a white dwarf no longer undergoes fusion reactions, it lacks a heat source to support it against gravitational collapse. Instead, it is supported only by electron degeneracy pressure, causing it to be extremely dense. The physics of degeneracy yields a maximum mass for a non-rotating white dwarf, the Chandrasekhar limit— approximately 1.44 times M_☉— beyond which electron degeneracy pressure cannot support it. A carbon–oxygen white dwarf which approaches this limit, typically by mass transfer from a companion star, may explode as a Type Ia supernova via a process known as carbon detonation;^[1]^[5] SN 1006 is a likely example.

A white dwarf, very hot when it forms, gradually cools as it radiates its energy. This radiation, which initially has a high color temperature, lessens and reddens over time. Eventually a white dwarf will cool enough that its material will begin to crystallize, starting with the core. No longer emitting significant heat or light, and it will become a cold black dwarf.^[5] Inasmuch as the length of time it takes for a white dwarf to reach this end state has been calculated to be longer than the current age of the known universe (approximately 13.8 billion years),^[10] it is thought that no black dwarfs exist.^[1]^[4] The oldest known white dwarfs still radiate at temperatures of a few thousand kelvins, which establishes an observational limit on the maximum possible age of the universe.^[11]

The first white dwarf discovered was in the triple star system of 40 Eridani, which contains the relatively bright main sequence star 40 Eridani A, orbited at a distance by the closer binary system of the white dwarf 40 Eridani B and the main sequence red dwarf 40 Eridani C. The pair 40 Eridani B/C was discovered by William Herschel on 31 January 1783.^[12] In 1910, Henry Norris Russell, Edward Charles Pickering and Williamina Fleming discovered that, despite being a dim star, 40 Eridani B was of spectral type A, or white.^[13] In 1939, Russell looked back on the discovery noted that Pickering had suggested that such exceptions lead to breakthroughs and in this case it lead to the discovery of white dwarfs.^[3]^: 1 The spectral type of 40 Eridani B was officially described in 1914 by Walter Adams.^[14]

The white dwarf companion of Sirius, Sirius B, was next to be discovered. During the nineteenth century, positional measurements of some stars became precise enough to measure small changes in their location. Friedrich Bessel used position measurements to determine that the stars Sirius (α Canis Majoris) and Procyon (α Canis Minoris) were changing their positions periodically. In 1844 he predicted that both stars had unseen companions.^[15]

Bessel roughly estimated the period of the companion of Sirius to be about half a century;^[15] C.A.F. Peters computed an orbit for it in 1851.^[16] It was not until 31 January 1862 that Alvan Graham Clark observed a previously unseen star close to Sirius, later identified as the predicted companion.^[16] Walter Adams announced in 1915 that he had found the spectrum of Sirius B to be similar to that of Sirius.^[17]

In 1917, Adriaan van Maanen discovered van Maanen's Star, an isolated white dwarf.^[18] These three white dwarfs, the first discovered, are the so-called classical white dwarfs.^[3]^: 2 Eventually, many faint white stars that had high proper motion were found, indicating that they could be suspected to be low-luminosity stars close to the Earth, and hence white dwarfs. Willem Luyten appears to have been the first to use the term white dwarf when he examined this class of stars in 1922;^[13]^[19]^[20]^[21]^[22] the term was later popularized by Arthur Eddington.^[13]^[23] Despite these suspicions, the first non-classical white dwarf was not definitely identified until the 1930s. 18 white dwarfs had been discovered by 1939.^[3]^: 3 Luyten and others continued to search for white dwarfs in the 1940s. By 1950, over a hundred were known,^[24] and by 1999, over 2000 were known.^[25] Since then the Sloan Digital Sky Survey has found over 9000 white dwarfs, mostly new.^[26]

Although white dwarfs are known with estimated masses as low as 0.17 M_☉^[27] and as high as 1.33 M_☉,^[28] the mass distribution is strongly peaked at 0.6 M_☉, and the majority lie between 0.5 and 0.7 M_☉.^[28] The estimated radii of observed white dwarfs are typically 0.8–2% the radius of the Sun;^[29] this is comparable to the Earth's radius of approximately 0.9% solar radius. A white dwarf, then, packs mass comparable to the Sun's into a volume that is typically a million times smaller than the Sun's; the average density of matter in a white dwarf must therefore be, very roughly, 1000000 times greater than the average density of the Sun, or approximately 10⁶ g/cm³, or 1 tonne per cubic centimetre.^[1] A typical white dwarf has a density of between 10⁴ and 10⁷ g/cm³. White dwarfs are composed of one of the densest forms of matter known, surpassed only by other compact stars such as neutron stars and the hypothetical quark stars.^[30]^[31]

White dwarfs were found to be extremely dense soon after their discovery. If a star is in a binary system, as is the case for Sirius B or 40 Eridani B, it is possible to estimate its mass from observations of the binary orbit. This was done for Sirius B by 1910,^[32] yielding a mass estimate of 0.94 M_☉, which compares well with a more modern estimate of 1.00 M_☉.^[33] Since hotter bodies radiate more energy than colder ones, a star's surface brightness can be estimated from its effective surface temperature, and that from its spectrum. If the star's distance is known, its absolute luminosity can also be estimated. From the absolute luminosity and distance, the star's surface area and its radius can be calculated. Reasoning of this sort led to the realization, puzzling to astronomers at the time, that due to their relatively high temperature and relatively low absolute luminosity, Sirius B and 40 Eridani B must be very dense. When Ernst Öpik estimated the density of a number of visual binary stars in 1916, he found that 40 Eridani B had a density of over 25000 times that of the Sun, which was so high that he called it "impossible".^[34] As Arthur Eddington put it later, in 1927:^[35]^: 50

We learn about the stars by receiving and interpreting the messages which their light brings to us. The message of the companion of Sirius when it was decoded ran: "I am composed of material 3000 times denser than anything you have ever come across; a ton of my material would be a little nugget that you could put in a matchbox." What reply can one make to such a message? The reply which most of us made in 1914 was — "Shut up. Don't talk nonsense."

As Eddington pointed out in 1924, densities of this order implied that, according to the theory of general relativity, the light from Sirius B should be gravitationally redshifted.^[23] This was confirmed when Adams measured this redshift in 1925.^[36]

More information Material, Density [kg/m3] ...

Material	Density [kg/m³]	Notes
Supermassive black hole	c. 1000^[37]	Critical density of a black hole of around 10⁸ solar masses.
Water (liquid)	1000	At STP
Osmium	22610	Near room temperature
The core of the Sun	c. 150000
White dwarf	1×10⁹^[1]
Atomic nuclei	2.3×10¹⁷^[38]	Does not depend strongly on size of nucleus
Neutron star core	8.4×10¹⁶ – 1×10¹⁸
Small black hole	2×10³⁰^[39]	Critical density of an Earth-mass black hole.

Close

Such densities are possible because white dwarf material is not composed of atoms joined by chemical bonds, but rather consists of a plasma of unbound nuclei and electrons. There is therefore no obstacle to placing nuclei closer than normally allowed by electron orbitals limited by normal matter.^[23] Eddington wondered what would happen when this plasma cooled and the energy to keep the atoms ionized was no longer sufficient.^[40] This paradox was resolved by R. H. Fowler in 1926 by an application of the newly devised quantum mechanics. Since electrons obey the Pauli exclusion principle, no two electrons can occupy the same state, and they must obey Fermi–Dirac statistics, also introduced in 1926 to determine the statistical distribution of particles that satisfy the Pauli exclusion principle.^[41] At zero temperature, therefore, electrons cannot all occupy the lowest-energy, or ground, state; some of them would have to occupy higher-energy states, forming a band of lowest-available energy states, the Fermi sea. This state of the electrons, called degenerate, meant that a white dwarf could cool to zero temperature and still possess high energy.^[40]^[42]

Compression of a white dwarf will increase the number of electrons in a given volume. Applying the Pauli exclusion principle, this will increase the kinetic energy of the electrons, thereby increasing the pressure.^[40]^[43] This electron degeneracy pressure supports a white dwarf against gravitational collapse. The pressure depends only on density and not on temperature. Degenerate matter is relatively compressible; this means that the density of a high-mass white dwarf is much greater than that of a low-mass white dwarf and that the radius of a white dwarf decreases as its mass increases.^[1]

The existence of a limiting mass that no white dwarf can exceed without collapsing to a neutron star is another consequence of being supported by electron degeneracy pressure. Such limiting masses were calculated for cases of an idealized, constant density star in 1929 by Wilhelm Anderson^[44] and in 1930 by Edmund C. Stoner.^[45] This value was corrected by considering hydrostatic equilibrium for the density profile, and the presently known value of the limit was first published in 1931 by Subrahmanyan Chandrasekhar in his paper "The Maximum Mass of Ideal White Dwarfs".^[46] For a non-rotating white dwarf, it is equal to approximately $5.7 M ☉ / μ e 2$ , where $μ e$ is the average molecular weight per electron of the star.^[47]^: eqn.(63) As the carbon-12 and oxygen-16 that predominantly compose a carbon–oxygen white dwarf both have atomic numbers equal to half their atomic weight, one should take $μ e$ equal to 2 for such a star,^[42] leading to the commonly quoted value of 1.4 M_☉. (Near the beginning of the 20th century, there was reason to believe that stars were composed chiefly of heavy elements,^[45]^: 955 so, in his 1931 paper, Chandrasekhar set the average molecular weight per electron, $μ e$ , equal to 2.5, giving a limit of 0.91 M_☉.) Together with William Alfred Fowler, Chandrasekhar received the Nobel Prize for this and other work in 1983.^[48] The limiting mass is now called the Chandrasekhar limit.^[49]

If a carbon-oxygen white dwarf accreted enough matter to reach the Chandrasekhar limit of about 1.44 solar masses (for a non-rotating star), it would no longer be able to support the bulk of its mass through electron degeneracy pressure^[50] and, in the absence of nuclear reactions, would begin to collapse.^[51]^[52] However, the current view is that this limit is not normally attained; increasing temperature and density inside the core ignite carbon fusion as the star approaches the limit (to within about 1%) before collapse is initiated.^[52]^[53] In contrast, for a core primarily composed of oxygen, neon and magnesium, the collapsing white dwarf will typically form a neutron star. In this case, only a fraction of the star's mass will be ejected during the collapse.^[50]

If a white dwarf star accumulates sufficient material from a stellar companion to raise its core temperature enough to ignite carbon fusion, it will undergo runaway nuclear fusion, completely disrupting it. There are three avenues by which this detonation is theorised to happen: stable accretion of material from a companion, the collision of two white dwarfs, or accretion that causes ignition in a shell that then ignites the core. The dominant mechanism by which type Ia supernovae are produced remains unclear.^[54] Despite this uncertainty in how type Ia supernovae are produced, type Ia supernovae have very uniform properties and are useful standard candles over intergalactic distances. Some calibrations are required to compensate for the gradual change in properties or different frequencies of abnormal luminosity supernovae at high redshift, and for small variations in brightness identified by light curve shape or spectrum.^[55]^[56]^[57]

White dwarfs have low luminosity and therefore occupy a strip at the bottom of the Hertzsprung–Russell diagram, a graph of stellar luminosity versus color or temperature. They should not be confused with low-luminosity objects at the low-mass end of the main sequence, such as the hydrogen-fusing red dwarfs, whose cores are supported in part by thermal pressure,^[58] or the even lower-temperature brown dwarfs.^[59]

Mass–radius relationship

The relationship between the mass and radius of low-mass white dwarfs can be estimated using the nonrelativistic Fermi gas equation of state, which gives^[42]

R\approx {\frac {N^{5/3}\hbar ^{2}}{2m_{\text{e}}GM^{1/3}}},

where $R$ is the radius, $M$ is the total mass of the star, $N$ is the number of electrons per unit mass (dependent only on composition), $m e$ is the electron mass, $\hbar$ is the reduced Planck constant, and $G$ is the gravitational constant.

Since this analysis uses the non-relativistic formula $T = p 2 / 2 m$ for the kinetic energy, it is non-relativistic. When the electron velocity in a white dwarf is close to the speed of light, the kinetic energy formula approaches $T = pc$ where $c$ is the speed of light, and it can be shown that there is no stable equilibrium in the ultrarelativistic limit. In particular, this analysis yields the maximum mass of a white dwarf, which is^[42]

M_{\rm {limit}}\approx N^{2}\left({\frac {\hbar c}{G}}\right)^{3/2}.

For a more accurate computation of the mass-radius relationship and limiting mass of a white dwarf, one must compute the equation of state that describes the relationship between density and pressure in the white dwarf material. If the density and pressure are both set equal to functions of the radius from the center of the star, the system of equations consisting of the hydrostatic equation together with the equation of state can then be solved to find the structure of the white dwarf at equilibrium. In the non-relativistic case, the radius is inversely proportional to the cube root of the mass.^[47]^: eqn.(80) Relativistic corrections will alter the result so that the radius becomes zero at a finite value of the mass. This is the limiting value of the mass – called the Chandrasekhar limit – at which the white dwarf can no longer be supported by electron degeneracy pressure. The graph on the right shows the result of such a computation. It shows how radius varies with mass for non-relativistic (blue curve) and relativistic (green curve) models of a white dwarf. Both models treat the white dwarf as a cold Fermi gas in hydrostatic equilibrium. The average molecular weight per electron, $μ e$ , has been set equal to 2. Radius is measured in standard solar radii and mass in standard solar masses.^[47]^[60]

These computations all assume that the white dwarf is non-rotating. If the white dwarf is rotating, the equation of hydrostatic equilibrium must be modified to take into account the centrifugal pseudo-force arising from working in a rotating frame.^[61] For a uniformly rotating white dwarf, the limiting mass increases only slightly. If the star is allowed to rotate nonuniformly, and viscosity is neglected, then, as was pointed out by Fred Hoyle in 1947,^[62] there is no limit to the mass for which it is possible for a model white dwarf to be in static equilibrium. Not all of these model stars will be dynamically stable.^[63]

Rotating white dwarfs and the estimates of their diameter in terms of the angular velocity of rotation has been treated in the rigorous mathematical literature.^[64] The fine structure of the free boundary of white dwarfs has also been analysed mathematically rigorously.^[65]

Radiation and cooling

The degenerate matter that makes up the bulk of a white dwarf has a very low opacity, because any absorption of a photon requires that an electron must transition to a higher empty state, which may not be possible as the energy of the photon may not be a match for the possible quantum states available to that electron, hence radiative heat transfer within a white dwarf is low; it does, however, have a high thermal conductivity. As a result, the interior of the white dwarf maintains an almost uniform temperature as it cools down, starting at approximately 10⁸ K shortly after the formation of the white dwarf and reaching less than 10⁶ K for the coolest known white dwarfs.^[30] An outer shell of non-degenerate matter sits on top of the degenerate core. The outermost layers, which are cooler than the interior, radiate roughly as a black body. A white dwarf remains visible for a long time, as its tenuous outer atmosphere slowly radiates the thermal content of the degenerate interior.^[30]

The visible radiation emitted by white dwarfs varies over a wide color range, from the whitish-blue color of an O-, B- or A-type main sequence star to the yellow-orange of a late K- or early M-type star.^[66] White dwarf effective surface temperatures extend from over 150000 K^[25] to barely under 4000 K.^[67]^[68] In accordance with the Stefan–Boltzmann law, luminosity increases with increasing surface temperature (proportional to T⁴); this surface temperature range corresponds to a luminosity from over 100 times that of the Sun to under 1⁄10000 that of the Sun.^[68] Hot white dwarfs, with surface temperatures in excess of 30000 K, have been observed to be sources of soft (i.e., lower-energy) X-rays. This enables the composition and structure of their atmospheres to be studied by soft X-ray and extreme ultraviolet observations.^[69]

White dwarfs also radiate neutrinos through the Urca process.^[70] This process has more effect on hotter and younger white dwarfs. Because neutrinos can pass easily through stellar plasma, they can drain energy directly from the dwarf's interior; this mechanism is the dominant contribution to cooling for approximately the first 20 million years of a white dwarf's existence.^[30]

As was explained by Leon Mestel in 1952, unless the white dwarf accretes matter from a companion star or other source, its radiation comes from its stored heat, which is not replenished.^[71]^[72]^: §2.1 White dwarfs have an extremely small surface area to radiate this heat from, so they cool gradually, remaining hot for a long time.^[5] As a white dwarf cools, its surface temperature decreases, the radiation that it emits reddens, and its luminosity decreases. Since the white dwarf has no energy sink other than radiation, it follows that its cooling slows with time. The rate of cooling has been estimated for a carbon white dwarf of 0.59 M_☉ with a hydrogen atmosphere. After initially taking approximately 1.5 billion years to cool to a surface temperature of 7140 K, cooling approximately 500 more kelvins to 6590 K takes around 0.3 billion years, but the next two steps of around 500 kelvins (to 6030 K and 5550 K) take first 0.4 and then 1.1 billion years.^[73]^: Table 2

Most observed white dwarfs have relatively high surface temperatures, between 8000 K and 40000 K.^[26]^[74] A white dwarf, though, spends more of its lifetime at cooler temperatures than at hotter temperatures, so we should expect that there are more cool white dwarfs than hot white dwarfs. Once we adjust for the selection effect that hotter, more luminous white dwarfs are easier to observe, we do find that decreasing the temperature range examined results in finding more white dwarfs.^[75] This trend stops when we reach extremely cool white dwarfs; few white dwarfs are observed with surface temperatures below 4000 K,^[76] and one of the coolest so far observed, WD J2147–4035, has a surface temperature of approximately 3050 K.^[77] The reason for this is that the Universe's age is finite;^[78]^[79] there has not been enough time for white dwarfs to cool below this temperature. The white dwarf luminosity function can therefore be used to find the time when stars started to form in a region; an estimate for the age of our galactic disk found in this way is 8 billion years.^[75] A white dwarf will eventually, in many trillions of years, cool and become a non-radiating black dwarf in approximate thermal equilibrium with its surroundings and with the cosmic background radiation. No black dwarfs are thought to exist yet.^[1]

At very low temperatures (<4000 K) white dwarfs with hydrogen in their atmosphere will be affected by collision induced absoption (CIA) of hydrogen molecules colliding with helium atoms. This affects the optical red and infrared brightness of white dwarfs with a hydrogen or mixed hydrogen-helium atmosphere. This makes old white dwarfs with this kind of atmosphere bluer than the main cooling sequence. White dwarfs with hydrogen-poor atmospheres, such as WD J2147–4035, are less affected by CIA and therefore have a yellow to orange color.^[80]^[77]

White dwarf core material is a completely ionized plasma – a mixture of nuclei and electrons – that is initially in a fluid state. It was theoretically predicted in the 1960s that at a late stage of cooling, it should crystallize into a solid state, starting at its center.^[81] The crystal structure is thought to be a body-centered cubic lattice.^[4]^[82] In 1995 it was suggested that asteroseismological observations of pulsating white dwarfs yielded a potential test of the crystallization theory,^[83] and in 2004, observations were made that suggested approximately 90% of the mass of BPM 37093 had crystallized.^[84]^[85]^[86] Other work gives a crystallized mass fraction of between 32% and 82%.^[87] As a white dwarf core undergoes crystallization into a solid phase, latent heat is released, which provides a source of thermal energy that delays its cooling.^[88] Another possible mechanism that was suggested to explain the seeming delay in the cooling of some types of white dwarfs is a solid–liquid distillation process: the crystals formed in the core are buoyant and float up, thereby displacing heavier liquid downward, thus causing a net release of gravitational energy.^[89] Chemical fractionation between the ionic species in the plasma mixture can release a similar or even greater amount of energy.^[90]^[91]^[92] This energy release was first confirmed in 2019 after the identification of a pile up in the cooling sequence of more than 15000 white dwarfs observed with the Gaia satellite.^[93]

Low-mass helium white dwarfs (mass < 0.20 M_☉), often referred to as extremely low-mass white dwarfs (ELM WDs), are formed in binary systems. As a result of their hydrogen-rich envelopes, residual hydrogen burning via the CNO cycle may keep these white dwarfs hot for hundreds of millions of years.^[94] In addition, they remain in a bloated proto-white dwarf stage for up to 2 Gyr before they reach the cooling track.^[95]

Atmosphere and spectra

Although most white dwarfs are thought to be composed of carbon and oxygen, spectroscopy typically shows that their emitted light comes from an atmosphere that is observed to be either hydrogen or helium dominated. The dominant element is usually at least 1000 times more abundant than all other elements. As explained by Schatzman in the 1940s, the high surface gravity is thought to cause this purity by gravitationally separating the atmosphere so that heavy elements are below and the lighter above.^[97]^[98]^{: §§5–6} This atmosphere, the only part of the white dwarf visible to us, is thought to be the top of an envelope that is a residue of the star's envelope in the AGB phase and may also contain material accreted from the interstellar medium. The envelope is believed to consist of a helium-rich layer with mass no more than 1⁄100 of the star's total mass, which, if the atmosphere is hydrogen-dominated, is overlain by a hydrogen-rich layer with mass approximately 1⁄10000 of the star's total mass.^[68]^[99]^{: §§4–5}

Although thin, these outer layers determine the thermal evolution of the white dwarf. The degenerate electrons in the bulk of a white dwarf conduct heat well. Most of a white dwarf's mass is therefore at almost the same temperature (isothermal), and it is also hot: a white dwarf with surface temperature between 8000 K and 16000 K will have a core temperature between approximately 5000000 K and 20000000 K. The white dwarf is kept from cooling very quickly only by its outer layers' opacity to radiation.^[68]

More information Primary and secondary features, Secondary features only ...

White dwarf spectral types^[25]
Primary and secondary features
A	H lines present
B	He I lines
C	Continuous spectrum; no lines
O	He II lines, accompanied by He I or H lines
Z	Metal lines
Q	Carbon lines present
X	Unclear or unclassifiable spectrum
Secondary features only
P	Magnetic white dwarf with detectable polarization
H	Magnetic white dwarf without detectable polarization
E	Emission lines present
V	Variable

Close

The first attempt to classify white dwarf spectra appears to have been by G. P. Kuiper in 1941,^[66]^[100] and various classification schemes have been proposed and used since then.^[101]^[102] The system currently in use was introduced by Edward M. Sion, Jesse L. Greenstein and their coauthors in 1983 and has been subsequently revised several times. It classifies a spectrum by a symbol that consists of an initial D, a letter describing the primary feature of the spectrum followed by an optional sequence of letters describing secondary features of the spectrum (as shown in the adjacent table), and a temperature index number, computed by dividing 50400 K by the effective temperature. For example, a white dwarf with only He I lines in its spectrum and an effective temperature of 15000 K could be given the classification of DB3, or, if warranted by the precision of the temperature measurement, DB3.5. Likewise, a white dwarf with a polarized magnetic field, an effective temperature of 17000 K, and a spectrum dominated by He I lines that also had hydrogen features could be given the classification of DBAP3. The symbols "?" and ":" may also be used if the correct classification is uncertain.^[25]^[66]

White dwarfs whose primary spectral classification is DA have hydrogen-dominated atmospheres. They make up the majority, approximately 80%, of all observed white dwarfs.^[68] The next class in number is of DBs, approximately 16%.^[103] The hot, above 15000 K, DQ class (roughly 0.1%) have carbon-dominated atmospheres.^[104] Those classified as DB, DC, DO, DZ, and cool DQ have helium-dominated atmospheres. Assuming that carbon and metals are not present, which spectral classification is seen depends on the effective temperature. Between approximately 100000 K to 45000 K, the spectrum will be classified DO, dominated by singly ionized helium. From 30000 K to 12000 K, the spectrum will be DB, showing neutral helium lines, and below about 12000 K, the spectrum will be featureless and classified DC.^[99]^: §2.4^[68]

Molecular hydrogen (H₂) has been detected in spectra of the atmospheres of some white dwarfs.^[105] While theoretical work suggests that some types of white dwarfs may have stellar corona, searches at X-ray and radio wavelengths, where coronae are most easily detected, have been unsuccessful.^[106]^[107]

Metal-rich white dwarfs

Around 25–33% of white dwarfs have metal lines in their spectra, which is notable because any heavy elements in a white dwarf should sink into the star's interior in just a small fraction of the star's lifetime.^[108] The prevailing explanation for metal-rich white dwarfs is that they have recently accreted rocky planetesimals.^[108] The bulk composition of the accreted object can be measured from the strengths of the metal lines. For example, a 2015 study of the white dwarf Ton 345 concluded that its metal abundances were consistent with those of a differentiated, rocky planet whose mantle had been eroded by the host star's wind during its asymptotic giant branch phase.^[109]

Magnetic field

Magnetic fields in white dwarfs with a strength at the surface of c. 1 million gauss (100 teslas) were predicted by P. M. S. Blackett in 1947 as a consequence of a physical law he had proposed, which stated that an uncharged, rotating body should generate a magnetic field proportional to its angular momentum.^[110] This putative law, sometimes called the Blackett effect, was never generally accepted, and by the 1950s even Blackett felt it had been refuted.^[111]^: 39–43 In the 1960s, it was proposed that white dwarfs might have magnetic fields due to conservation of total surface magnetic flux that existed in its progenitor star phase.^[112] A surface magnetic field of c. 100 gauss (0.01 T) in the progenitor star would thus become a surface magnetic field of c. 100 × 100² = 1 million gauss (100 T) once the star's radius had shrunk by a factor of 100.^[98]^: §8^[113]^: 484 The first magnetic white dwarf to be discovered was GJ 742 (also known as GRW +70 8247), which was identified by James Kemp, John Swedlund, John Landstreet and Roger Angel in 1970 to host a magnetic field by its emission of circularly polarized light.^[114] It is thought to have a surface field of approximately 300 million gauss (30 kT).^[98]^: §8

Since 1970, magnetic fields have been discovered in well over 200 white dwarfs, ranging from 2×10³ to 10⁹ gauss (0.2 T to 100 kT).^[115] Many of the presently known magnetic white dwarfs are identified by low-resolution spectroscopy, which is able to reveal the presence of a magnetic field of 1 megagauss or more. Thus the basic identification process also sometimes results in discovery of magnetic fields.^[116] White dwarf magnetic fields may also be measured without spectral lines, using the techniques of broadband circular polarimetry, or maybe through measurement of their frequencies of radio emission via the electron cyclotron maser.^[107] It has been estimated that at least 10% of white dwarfs have fields in excess of 1 million gauss (100 T).^[117]^[118] The magnetic fields in a white dwarf may allow for the existence of a new type of chemical bond, perpendicular paramagnetic bonding, in addition to ionic and covalent bonds, though detecting molecules bonded in this way is expected to be difficult.^[119]

The highly magnetized white dwarf in the binary system AR Scorpii was identified in 2016 as the first pulsar in which the compact object is a white dwarf instead of a neutron star.^[120] A second white dwarf pulsar was discovered in 2023.^[121]

Types of pulsating white dwarf^[122]^[123]^{: §§1.1, 1.2}
DAV (GCVS: ZZA)	DA spectral type, having only hydrogen absorption lines in its spectrum
DBV (GCVS: ZZB)	DB spectral type, having only helium absorption lines in its spectrum
GW Vir (GCVS: ZZO)	Atmosphere mostly C, He and O; may be divided into DOV and PNNV stars

Early calculations suggested that there might be white dwarfs whose luminosity varied with a period of around 10 seconds, but searches in the 1960s failed to observe this.^[98]^: §7.1.1^[124] The first variable white dwarf found was HL Tau 76; in 1965 and 1966, and was observed to vary with a period of approximately 12.5 minutes.^[125] The reason for this period being longer than predicted is that the variability of HL Tau 76, like that of the other pulsating variable white dwarfs known, arises from non-radial gravity wave pulsations.^[98]^: §7 Known types of pulsating white dwarf include the DAV, or ZZ Ceti, stars, including HL Tau 76, with hydrogen-dominated atmospheres and the spectral type DA;^[98]^{: 891, 895} DBV, or V777 Her, stars, with helium-dominated atmospheres and the spectral type DB;^[68]^: 3525 and GW Vir stars, sometimes subdivided into DOV and PNNV stars, with atmospheres dominated by helium, carbon, and oxygen.^[123]^[126] GW Vir stars are not, strictly speaking, white dwarfs, but are stars that are in a position on the Hertzsprung–Russell diagram between the asymptotic giant branch and the white dwarf region. They may be called pre-white dwarfs.^[123]^[127] These variables all exhibit small (1%–30%) variations in light output, arising from a superposition of vibrational modes with periods of hundreds to thousands of seconds. Observation of these variations gives asteroseismological evidence about the interiors of white dwarfs.^[128]

White dwarfs are thought to represent the end point of stellar evolution for main-sequence stars with masses from about 0.07 to 10 M_☉.^[4]^[129] The composition of the white dwarf produced will depend on the initial mass of the star. Current galactic models suggest the Milky Way galaxy currently contains about ten billion white dwarfs.^[130]

Stars with very low mass

If the mass of a main-sequence star is lower than approximately half a solar mass, it will never become hot enough to ignite and fuse helium in its core.^[131] It is thought that, over a lifespan that considerably exceeds the age of the universe (c. 13.8 billion years),^[10] such a star will eventually burn all its hydrogen, for a while becoming a blue dwarf, and end its evolution as a helium white dwarf composed chiefly of helium-4 nuclei.^[132] Due to the very long time this process takes, it is not thought to be the origin of the observed helium white dwarfs. Rather, they are thought to be mostly the product of mass loss in binary systems.^[5]^[7]^[8]^[133]^[134]^[135] Proposals to explain those helium white dwarfs that are not part of binary systems include mass loss due to a large planetary companion, stars being stripped of material by companions exploding as supernovae, and various types of stellar mergers.^[136]^[137]

Stars with low to medium mass

If the mass of a main-sequence star is between 0.5 and 8 M_☉,^[131]^[138] its core will become sufficiently hot to fuse helium into carbon and oxygen via the triple-alpha process, but it will never become sufficiently hot to fuse carbon into neon. Near the end of the period in which it undergoes fusion reactions, such a star will have a carbon–oxygen core that does not undergo fusion reactions, surrounded by an inner helium-burning shell and an outer hydrogen-burning shell. On the Hertzsprung–Russell diagram, it will be found on the asymptotic giant branch. It will then expel most of its outer material, creating a planetary nebula, until only the carbon–oxygen core is left. This process is responsible for the carbon–oxygen white dwarfs that form the vast majority of observed white dwarfs.^[133]^[139]^[140]

Stars with medium to high mass

If a star is massive enough, its core will eventually become sufficiently hot to fuse carbon to neon, and then to fuse neon to iron. Such a star will not become a white dwarf, because the mass of its central, non-fusing core, initially supported by electron degeneracy pressure, will eventually exceed the largest possible mass supportable by degeneracy pressure. At this point the core of the star will collapse and it will explode in a core-collapse supernova that will leave behind a remnant neutron star, black hole, or possibly a more exotic form of compact star.^[129]^[141] Some main-sequence stars, of perhaps 8 to 10 M_☉, although sufficiently massive to fuse carbon to neon and magnesium, may be insufficiently massive to fuse neon. Such a star may leave a remnant white dwarf composed chiefly of oxygen, neon, and magnesium, provided that its core does not collapse, and provided that fusion does not proceed so violently as to blow apart the star in a supernova.^[142]^[138] Although a few white dwarfs have been identified that may be of this type, most evidence for the existence of such comes from the novae called ONeMg or neon novae. The spectra of these novae exhibit abundances of neon, magnesium, and other intermediate-mass elements that appear to be only explicable by the accretion of material onto an oxygen–neon–magnesium white dwarf.^[6]^[143]^[144]

Type Iax supernova

Type Iax supernovae, that involve helium accretion by a white dwarf, have been proposed to be a channel for transformation of this type of stellar remnant. In this scenario, the carbon detonation produced in a Type Ia supernova is too weak to destroy the white dwarf, expelling just a small part of its mass as ejecta, but produces an asymmetric explosion that kicks the star, often known as a zombie star, to the high speeds of a hypervelocity star. The matter processed in the failed detonation is re-accreted by the white dwarf with the heaviest elements such as iron falling to its core where it accumulates.^[145] These iron-core white dwarfs would be smaller than the carbon–oxygen kind of similar mass and would cool and crystallize faster than those.^[146]

Artist's concept of white dwarf aging

A white dwarf is stable once formed and will continue to cool almost indefinitely, eventually to become a black dwarf. Assuming that the universe continues to expand, it is thought that in 10¹⁹ to 10²⁰ years, the galaxies will evaporate as their stars escape into intergalactic space.^[147]^: §IIIA White dwarfs should generally survive galactic dispersion, although an occasional collision between white dwarfs may produce a new fusing star or a super-Chandrasekhar mass white dwarf that will explode in a Type Ia supernova.^[147]^{: §§IIIC, IV} The subsequent lifetime of white dwarfs is thought to be on the order of the hypothetical lifetime of the proton, known to be at least 10³⁴–10³⁵ years. Some grand unified theories predict a proton lifetime between 10³⁰ and 10³⁶ years. If these theories are not valid, the proton might still decay by complicated nuclear reactions or through quantum gravitational processes involving virtual black holes; in these cases, the lifetime is estimated to be no more than 10²⁰⁰ years. If protons do decay, the mass of a white dwarf will decrease very slowly with time as its nuclei decay, until it loses enough mass to become a nondegenerate lump of matter, and finally disappears completely.^[147]^: §IV

A white dwarf can also be cannibalized or evaporated by a companion star, causing the white dwarf to lose so much mass that it becomes a planetary mass object. The resultant object, orbiting the former companion, now host star, could be a helium planet or diamond planet.^[148]^[149]^[150]

A white dwarf's stellar and planetary system is inherited from its progenitor star and may interact with the white dwarf in various ways. There are several indications that a white dwarf has a remnant planetary system.

The most common observable evidence of a remnant planetary system is pollution of the spectrum of a white dwarf with metal absorption lines. 27–50% of white dwarfs show a spectrum polluted with metals,^[153] but these heavy elements settle out in the atmosphere of white dwarfs colder than 20000 K. The most widely accepted hypothesis is that this pollution comes from tidally disrupted rocky bodies.^[154]^[155] The first observation of a metal-polluted white dwarf was by van Maanen^[156] in 1917 at the Mount Wilson Observatory and is now recognized as the first evidence of exoplanets in astronomy.^[157] The white dwarf van Maanen 2 shows iron, calcium and magnesium in its atmosphere,^[158] but van Maanen misclassified it as the faintest F-type star based on the calcium H- and K-lines.^[159] The nitrogen in white dwarfs is thought to come from nitrogen-ice of extrasolar Kuiper Belt objects, the lithium is thought to come from accreted crust material and the beryllium is thought to come from exomoons.^[157]

A less common observable evidence is infrared excess due to a flat and optically thick debris disk, which is found in around 1%–4% of white dwarfs.^[155] The first white dwarf with infrared excess was discovered by Zuckerman and Becklin in 1987 in the near-infrared around Giclas 29-38^[160] and later confirmed as a debris disk.^[161] White dwarfs hotter than 27000 K sublimate all the dust formed by tidally disrupting a rocky body, preventing the formation of a debris disk. In colder white dwarfs, a rocky body might be tidally disrupted near the Roche radius and forced into a circular orbit by the Poynting–Robertson drag, which is stronger for less massive white dwarfs. The Poynting–Robertson drag will also cause the dust to orbit closer and closer towards the white dwarf, until it will eventually sublimate and the disk will disappear. A debris disk will have a lifetime of around a few million years for white dwarfs hotter than 10000 K. Colder white dwarfs can have disk-lifetimes of a few 10 million years, which is enough time to tidally disrupt a second rocky body and forming a second disk around a white dwarf, such as the two rings around LSPM J0207+3331.^[162]

The least common observable evidence of planetary systems are detected major or minor planets. Only a handful of giant planets and a handful of minor planets are known around white dwarfs.^[163]^[164]

Exoplanet orbits WD 1856+534

(NASA; video; 2:10)

Infrared spectroscopic observations made by NASA's Spitzer Space Telescope of the central star of the Helix Nebula suggest the presence of a dust cloud, which may be caused by cometary collisions. It is possible that infalling material from this may cause X-ray emission from the central star.^[165]^[166] Similarly, observations made in 2004 indicated the presence of a dust cloud around the young (estimated to have formed from its AGB progenitor about 500 million years ago) white dwarf G29-38, which may have been created by tidal disruption of a comet passing close to the white dwarf.^[161] Some estimations based on the metal content of the atmospheres of the white dwarfs consider that at least 15% of them may be orbited by planets or asteroids, or at least their debris.^[167] Another suggested idea is that white dwarfs could be orbited by the stripped cores of rocky planets, that would have survived the red giant phase of their star but losing their outer layers and, given those planetary remnants would likely be made of metals, to attempt to detect them looking for the signatures of their interaction with the white dwarf's magnetic field.^[168] Other suggested ideas of how white dwarfs are polluted with dust involve the scattering of asteroids by planets^[169]^[170]^[171] or via planet-planet scattering.^[172] Liberation of exomoons from their host planet could cause white dwarf pollution with dust. Either the liberation could cause asteroids to be scattered towards the white dwarf or the exomoon could be scattered into the Roche radius of the white dwarf.^[173] The mechanism behind the pollution of white dwarfs in binaries was also explored as these systems are more likely to lack a major planet, but this idea cannot explain the presence of dust around single white dwarfs.^[174] While old white dwarfs show evidence of dust accretion, white dwarfs older than ~1 billion years or >7000 K with dusty infrared excess were not detected^[175] until the discovery of LSPM J0207+3331 in 2018, which has a cooling age of ~3 billion years. The white dwarf shows two dusty components that are being explained with two rings with different temperatures.^[155]

Another possible way to detect planetary systems around white dwarfs is through their radio emissions. In 2004 and 2005, A. J. Willes and K. Wu hypothesized that when an exoplanet travels through the magnetosphere of a white dwarf, it may generate auroral radio emissions from the magnetic poles of the white dwarf, similar to how Io stimulates radio emissions from Jupiter. However, a search for such radio emission from nine white dwarfs by researchers using the Arecibo radio telescope did not find any so far.^[107]

The metal-rich white dwarf WD 1145+017 is the first white dwarf observed with a disintegrating minor planet that transits the star.^[176]^[177] The disintegration of the planetesimal generates a debris cloud that passes in front of the star every 4.5 hours, causing a 5-minute-long fade in the star's optical brightness.^[177] The depth of the transit is highly variable.^[177]

The giant planet WD J0914+1914b is being evaporated by the strong ultraviolet radiation of the hot white dwarf. Part of the evaporated material is being accreted in a gaseous disk around the white dwarf. The weak hydrogen line as well as other lines in the spectrum of the white dwarf revealed the presence of the giant planet.^[178]

The white dwarf WD 0145+234 shows brightening in the mid-infrared, seen in NEOWISE data. The brightening, not seen before 2018, may be due to the tidal disruption of an exoasteroid, the first time such an event has been observed.^[179]

WD 1856+534 is the first transiting major planet to be observed orbiting a white dwarf, and remains the only such example as of 2023.^[180]^[181] MOA-2010-BLG-477L, a white dwarf discovered thanks to a microlensing event, is also known to have a giant planet.^[182]^[164]

GD 140 and LAWD 37 are suspected to have giant exoplanets due to anomaly in the Hipparcos-Gaia proper motion. For GD 140 it is suspected to be a planet several times more massive than Jupiter and for LAWD 37 it is suspected to be a planet less massive than Jupiter.^[183]^[184] Additionally, WD 0141-675 was suspected to have a super-Jupiter with an orbital period of 33.65 days based on Gaia astrometry. This is remarkable because WD 0141-675 is polluted with metals and metal polluted white dwarfs have long be suspected to host giant planets that disturb the orbits of minor planets, causing the pollution.^[185] Both GD 140 and WD 0141 will be observed with JWST in cycle 2 with the aim to detect infrared excess caused by the planets.^[186] However, the planet candidate at WD 0141-675 was found to be a false positive caused by a software error.^[187]

A JWST survey of four metal polluted white dwarfs found two directly imaged exoplanet candidates with masses of 1–7 M_J. One orbits around WD 1202−232 (LP 852-7) and the other around WD 2105−82 (LAWD 83). If confirmed they would be the first directly imaged planets that likely formed from circumstellar disk material, representing a new population of directly imaged giant planets that are more similar to solar system giants in age and probably also in their atmosphere. Confirmation will be possible via the common proper motion method with JWST.^[164]

In 2024 it was discovered that the white dwarf in the PHL 5038AB system is polluted with calcium from rocky material. The white dwarf is orbited by a brown dwarf, which was discovered in 2009. This is seen as perhaps the first case of linking white dwarf pollution with the presence of a substellar object. It is thought that the orbits of planetesimals are being disrupted by the brown dwarf, causing the pollution of the white dwarf.^[188]

A search has been proposed for transits of hypothetical Earth-like planets around white dwarfs with surface temperatures of less than 10000 K. Such stars that could harbor a habitable zone at a distance of c. 0.005 to 0.02 AU that would last upwards of 3 billion years. This is so close that any habitable planets would be tidally locked. As a white dwarf has a size similar to that of a planet, these kinds of transits would produce strong eclipses.^[189]

Newer research casts some doubts on this idea, given that the close orbits of those hypothetical planets around their parent stars would subject them to strong tidal forces that could render them uninhabitable by triggering a greenhouse effect.^[190] Another suggested constraint to this idea is the origin of those planets. Leaving aside formation from the accretion disk surrounding the white dwarf, there are two ways a planet could end in a close orbit around stars of this kind: by surviving being engulfed by the star during its red giant phase, and then spiralling inward, or inward migration after the white dwarf has formed. The former case is implausible for low-mass bodies, as they are unlikely to survive being absorbed by their stars. In the latter case, the planets would have to expel so much orbital energy as heat, through tidal interactions with the white dwarf, that they would likely end as uninhabitable embers.^[191]

If a white dwarf is in a binary star system and is accreting matter from its companion, a variety of phenomena may occur, including novae and Type Ia supernovae. It may also be a super-soft x-ray source if it is able to take material from its companion fast enough to sustain fusion on its surface.^[192] On the other hand, phenomena in binary systems such as tidal interaction and star–disc interaction, moderated by magnetic fields or not, act on the rotation of accreting white dwarfs. In fact, the (securely known) fastest-spinning white dwarfs are members of binary systems (the fastest one being the white dwarf in CTCV J2056-3014).^[193] A close binary system of two white dwarfs can lose angular momentum and radiate energy in the form of gravitational waves, causing their mutual orbit to steadily shrink until the stars merge.^[194]^[195]

Type Ia supernovae

The mass of an isolated, nonrotating white dwarf cannot exceed the Chandrasekhar limit of ~ 1.4 M_☉. This limit may increase if the white dwarf is rotating rapidly and nonuniformly.^[196] White dwarfs in binary systems can accrete material from a companion star, increasing both their mass and their density. As their mass approaches the Chandrasekhar limit, this could theoretically lead to either the explosive ignition of fusion in the white dwarf or its collapse into a neutron star.^[50]

There are two models that might explain the progenitor systems of Type Ia supernovae: the single-degenerate model and the double-degenerate model. In the single-degenerate model, a carbon–oxygen white dwarf accretes mass and compresses its core by pulling mass from a companion non-degenerate star.^[197]^: 14 It is believed that compressional heating of the core leads to ignition of carbon fusion as the mass approaches the Chandrasekhar limit.^[197] Because the white dwarf is supported against gravity by quantum degeneracy pressure instead of by thermal pressure, adding heat to the star's interior increases its temperature but not its pressure, so the white dwarf does not expand and cool in response. Rather, the increased temperature accelerates the rate of the fusion reaction, in a runaway process that feeds on itself. The thermonuclear flame consumes much of the white dwarf in a few seconds, causing a Type Ia supernova explosion that obliterates the star.^[1]^[197]^[198] In another possible mechanism for Type Ia supernovae, the double-degenerate model, two carbon–oxygen white dwarfs in a binary system merge, creating an object with mass greater than the Chandrasekhar limit in which carbon fusion is then ignited.^[197]^: 14 In both cases, the white dwarfs are not expected to survive the Type Ia supernova.^[199]

The single-degenerate model was the favored mechanism for Type Ia supernovae, but now, because of observations, the double-degenerate model is thought to be the more likely scenario. Predicted rates of white dwarf-white dwarf mergers are comparable to the rate of Type Ia supernovae and would explain the lack of hydrogen in the spectra of Type Ia supernovae.^[200] However, the main mechanism for Type Ia supernovae remains an open question.^[201] In the single-degenerate scenario, the accretion rate onto the white dwarf needs to be within a narrow range dependent on its mass so that the hydrogen burning on the surface of the white dwarf is stable. If the accretion rate is too low, novae on the surface of the white dwarf will blow away accreted material. If it is too high, the white dwarf will expand and the white dwarf and companion star will be in a common envelope. This stops the growth of the white dwarf thus preventing it from reaching the Chandrasekhar limit and exploding.^[200] For the single-degenerate model its companion is expected to survive, but there is no strong evidence of such a star near Type Ia supernovae sites.^[199] In the double-degenerate scenario, white dwarfs need to be in very close binaries; otherwise their inspiral time is longer than the age of the universe. It is also likely that instead of a Type Ia supernova, the merger of two white dwarfs will lead to core-collapse. As a white dwarf accretes material quickly, the core can ignite off-center, which leads to gravitational instabilities that could create a neutron star.^[199]

The historical bright SN 1006 is thought to have been a Type Ia supernova from a white dwarf, possibly the merger of two white dwarfs.^[202] Tycho's Supernova of 1572 was also a type Ia supernova, and its remnant has been detected.^[203] WD 0810–353, a white dwarf 11 parsecs away from the Sun, is possibly a hypervelocity runaway ejected from a Type Ia supernova, though this has been disputed.^[204]^[205]

Post-common envelope binary

A post-common envelope binary (PCEB) is a binary consisting of a white dwarf or hot subdwarf and a closely tidally-locked red dwarf (in other cases this might be a brown dwarf instead of a red dwarf).^[206] These binaries form when the red dwarf is engulfed in the red giant phase. As the red dwarf orbits inside the common envelope, it is slowed down in the denser environment. This slowed orbital speed is compensated with a decrease of the orbital distance between the red dwarf and the core of the red giant. The red dwarf spirals inwards towards the core and might merge with the core. If this does not happen and instead the common envelope is ejected, then the binary ends up in a close orbit, consisting of a white dwarf and a red dwarf. This type of binary is called a post-common envelope binary. The evolution of the PCEB continues as the two dwarf stars orbit closer and closer due to magnetic braking and by releasing gravitational waves. The binary might then evolve into one of several dramatic outcomes: a high-field magnetic white dwarf, a white dwarf pulsar, a double-degenerate binary, or even a Type Ia supernova.^[207]^[208] Because a PCEB may evolve at some point into a cataclysmic variable, some of them are also called pre-cataclysmic variables.^[209]^[185]

Cataclysmic variables

Before accretion of material pushes a white dwarf close to the Chandrasekhar limit, accreted hydrogen-rich material on the surface may ignite in a less destructive type of thermonuclear explosion powered by hydrogen fusion. These surface explosions can be repeated as long as the white dwarf's core remains intact. This weaker kind of repetitive cataclysmic phenomenon is called a (classical) nova. Astronomers have also observed dwarf novae, which have smaller, more frequent luminosity peaks than the classical novae. These are thought to be caused by the release of gravitational potential energy when part of the accretion disc collapses onto the star, rather than through a release of energy due to fusion. In general, binary systems with a white dwarf accreting matter from a stellar companion are called cataclysmic variables. As well as novae and dwarf novae, several other classes of these variables are known, including polars and intermediate polars, both of which feature highly magnetic white dwarfs.^[1]^[197]^[210]^[211] Both fusion- and accretion-powered cataclysmic variables have been observed to be X-ray sources.^[211]

Other multiple-star systems

Other binaries include those that consist of a main sequence star (or giant) and a white dwarf. The binary Sirius AB is an example pair of this type.^[212] White dwarfs can also exist as binaries or multiple star systems that only consist of white dwarfs. An example of a resolved triple white dwarf system is WD J1953-1019, discovered with Gaia DR2 data.^[213] One interesting field is the study of remnant planetary systems around white dwarfs. It is expected that planets orbiting several AU from a star will survive the star's post-main-sequence transformation into a white dwarf. Moreover, white dwarfs, being much smaller and correspondingly less luminous than their progenitors, are less likely to outshine any bodies in orbit around them. This makes white dwarfs advantageous targets for direct-imaging searches for exoplanets and brown dwarfs. The first brown dwarf to be detected by direct imaging was the companion to the white dwarf GD 165 A, discovered in 1988.^[214] More recently, the white dwarf WD 0806−661 was found to have a cold companion body of substellar mass, variously described as a brown dwarf^[215]^[216] or an exoplanet.^[217]

More information Identifier, WD Number ...

White dwarfs within 25 light years^[218]
Identifier	WD Number	Distance [ly]	Type	Absolute magnitude	Mass [`M`_☉]	Luminosity [`L`_☉]	Age [Gyr]	Objects in system
Sirius B	0642–166	8.66	DA	11.18	0.98	0.0295	0.10	2
Procyon B	0736+053	11.46	DQZ	13.20	0.63	0.00049	1.37	2
Van Maanen 2	0046+051	14.07	DZ	14.09	0.68	0.00017	3.30	1
LP 145-141	1142–645	15.12	DQ	12.77	0.61	0.00054	1.29	1
40 Eridani B	0413-077	16.39	DA	11.27	0.59	0.0141	0.12	3
Stein 2051 B	0426+588	17.99	DC	13.43	0.69	0.00030	2.02	2
G 240-72	1748+708	20.26	DQ	15.23	0.81	0.000085	5.69	1
Gliese 223.2	0552–041	21.01	DZ	15.29	0.82	0.000062	7.89	1
Gliese 3991 B^[219]	1708+437	24.23	D??	> 15	0.5	< 0.000086	> 6	2

Close

Black dwarf – Theoretical stellar remnant
Brown dwarf – Type of substellar object larger than a planet
Chandrasekhar's white dwarf equation
Degenerate matter – Type of dense exotic matter in physics
List of white dwarfs
Neutron star – Collapsed core of a massive star
PG 1159 star
Planetary nebula – Type of emission nebula created by dying red giants
Robust associations of massive baryonic objects – Proposed type of star cluster
Stellar classification – Classification of stars based on spectral properties
Timeline of white dwarfs, neutron stars, and supernovae – Chronological list of developments in knowledge and records

[1]
Johnson, J. (2007). "Extreme stars: White dwarfs & neutron stars" (Lecture notes). Astronomy 162. Ohio State University. Archived from the original on 31 March 2012. Retrieved 17 October 2011.
[2]
Henry, T.J. (1 January 2009). "The one hundred nearest star systems". Research Consortium on Nearby Stars. Archived from the original on 12 November 2007. Retrieved 21 July 2010.
[3]
Evry L. Schatzman (1958). White Dwarfs. North-Holland Publishing Company. ISBN 978-0-598-58212-6.
[4]
Fontaine, G.; Brassard, P.; Bergeron, P. (2001). "The potential of white dwarf cosmochronology". Publications of the Astronomical Society of the Pacific. 113 (782): 409–435. Bibcode:2001PASP..113..409F. doi:10.1086/319535.
[5]
Richmond, M. "Late stages of evolution for low-mass stars". Lecture notes, Physics 230. Rochester Institute of Technology. Archived from the original on 4 September 2017. Retrieved 3 May 2007.
[6]
Werner, K.; Hammer, N.J.; Nagel, T.; Rauch, T.; Dreizler, S. (2005). On possible oxygen / neon white dwarfs: H1504+65 and the white dwarf donors in ultracompact X-ray binaries. 14th European Workshop on White Dwarfs. Vol. 334. p. 165. arXiv:astro-ph/0410690. Bibcode:2005ASPC..334..165W.
[7]
Liebert, James; Bergeron, P.; Eisenstein, D.; Harris, H. C.; Kleinman, S. J.; Nitta, A.; Krzesinski, J. (2004). "A helium white dwarf of extremely low mass". The Astrophysical Journal. 606 (2): L147. arXiv:astro-ph/0404291. Bibcode:2004ApJ...606L.147L. doi:10.1086/421462. S2CID 118894713.
[8]
"Cosmic weight loss: The lowest mass white dwarf" (Press release). Harvard-Smithsonian Center for Astrophysics. 17 April 2007. Archived from the original on 22 April 2007. Retrieved 20 April 2007.
[9]
Althaus, L. G.; Benvenuto, O. G. (March 1997). "Evolution of Helium White Dwarfs of Low and Intermediate Masses". The Astrophysical Journal. 477 (1): 313–334. Bibcode:1997ApJ...477..313A. doi:10.1086/303686.
[10]
Spergel, D.N.; Bean, R.; Doré, O.; Nolta, M.R.; Bennett, C.L.; Dunkley, J.; et al. (2007). "Wilkinson Microwave Anisotropy Probe (WMAP) three year results: Implications for cosmology". The Astrophysical Journal Supplement Series. 170 (2): 377–408. arXiv:astro-ph/0603449. Bibcode:2007ApJS..170..377S. doi:10.1086/513700. S2CID 1386346.
[11]
§3, Heger, A.; Fryer, C.L.; Woosley, S.E.; Langer, N.; Hartmann, D.H. (2003). "How massive single stars end their life". Astrophysical Journal. 591 (1): 288–300. arXiv:astro-ph/0212469. Bibcode:2003ApJ...591..288H. doi:10.1086/375341. S2CID 59065632.
[12]
Herschel, W. (1785). "Catalogue of Double Stars". Philosophical Transactions of the Royal Society of London. 75: 40–126. Bibcode:1785RSPT...75...40H. doi:10.1098/rstl.1785.0006. JSTOR 106749. S2CID 186209747.
[13]
Holberg, J. B. (2005). How degenerate stars came to be known as 'white dwarfs'. American Astronomical Society meeting 207. Vol. 207. p. 1503. Bibcode:2005AAS...20720501H.
[14]
Adams, W.S. (1914). "An A-type star of very low luminosity". Publications of the Astronomical Society of the Pacific. 26 (155): 198. Bibcode:1914PASP...26..198A. doi:10.1086/122337.
[15]
Bessel, F.W. (1844). "On the variations of the proper motions of Procyon and Sirius". Monthly Notices of the Royal Astronomical Society. 6 (11): 136–141. Bibcode:1844MNRAS...6R.136B. doi:10.1093/mnras/6.11.136a.
[16]
Flammarion, Camille (1877). "The companion of Sirius". Astronomical Register. 15: 186. Bibcode:1877AReg...15..186F.
[17]
Adams, W.S. (1915). "The spectrum of the companion of Sirius". Publications of the Astronomical Society of the Pacific. 27 (161): 236. Bibcode:1915PASP...27..236A. doi:10.1086/122440.
[18]
van Maanen, A. (1917). "Two faint stars with large proper motion". Publications of the Astronomical Society of the Pacific. 29 (172): 258. Bibcode:1917PASP...29..258V. doi:10.1086/122654.
[19]
Luyten, W.J. (1922). "The mean parallax of early-type stars of determined proper motion and apparent magnitude". Publications of the Astronomical Society of the Pacific. 34 (199): 156. Bibcode:1922PASP...34..156L. doi:10.1086/123176.
[20]
Luyten, W.J. (1922). "Note on some faint early-type stars with large proper motions". Publications of the Astronomical Society of the Pacific. 34 (197): 54. Bibcode:1922PASP...34...54L. doi:10.1086/123146.
[21]
Luyten, W.J. (1922). "Additional note on faint early-type stars with large proper motions". Publications of the Astronomical Society of the Pacific. 34 (198): 132. Bibcode:1922PASP...34..132L. doi:10.1086/123168.
[22]
Aitken, R.G. (1922). "Comet c 1922 (Baade)". Publications of the Astronomical Society of the Pacific. 34 (202): 353. Bibcode:1922PASP...34..353A. doi:10.1086/123244.
[23]
Eddington, A. S. (1924). "On the relation between the masses and luminosities of the stars". Monthly Notices of the Royal Astronomical Society. 84 (5): 308–333. Bibcode:1924MNRAS..84..308E. doi:10.1093/mnras/84.5.308.
[24]
Luyten, W.J. (1950). "The search for white dwarfs". The Astronomical Journal. 55: 86. Bibcode:1950AJ.....55...86L. doi:10.1086/106358.
[25]
McCook, George P.; Sion, Edward M. (1999). "A catalog of spectroscopically identified white dwarfs". The Astrophysical Journal Supplement Series. 121 (1): 1–130. Bibcode:1999ApJS..121....1M. doi:10.1086/313186.
[26]
Eisenstein, Daniel J.; Liebert, James; Harris, Hugh C.; Kleinman, S. J.; Nitta, Atsuko; Silvestri, Nicole; et al. (2006). "A catalog of spectroscopically confirmed white dwarfs from the Sloan Digital Sky Survey, data release 4". The Astrophysical Journal Supplement Series. 167 (1): 40–58. arXiv:astro-ph/0606700. Bibcode:2006ApJS..167...40E. doi:10.1086/507110. S2CID 13829139.
[27]
Kilic, M.; Allende Prieto, C.; Brown, Warren R.; Koester, D. (2007). "The lowest mass white dwarf". The Astrophysical Journal. 660 (2): 1451–1461. arXiv:astro-ph/0611498. Bibcode:2007ApJ...660.1451K. doi:10.1086/514327. S2CID 18587748.
[28]
Kepler, S.O.; Kleinman, S.J.; Nitta, A.; Koester, D.; Castanheira, B.G.; Giovannini, O.; Costa, A.F.M.; Althaus, L. (2007). "White dwarf mass distribution in the SDSS". Monthly Notices of the Royal Astronomical Society. 375 (4): 1315–1324. arXiv:astro-ph/0612277. Bibcode:2007MNRAS.375.1315K. doi:10.1111/j.1365-2966.2006.11388.x. S2CID 10892288.
[29]
Shipman, H.L. (1979). "Masses and radii of white-dwarf stars. III – Results for 110 hydrogen-rich and 28 helium-rich stars". The Astrophysical Journal. 228: 240. Bibcode:1979ApJ...228..240S. doi:10.1086/156841.
[30]
Saumon, Didier; Blouin, Simon; Tremblay, Pier-Emmanuel (November 2022). "Current challenges in the physics of white dwarf stars". Physics Reports. 988: 1–63. arXiv:2209.02846. Bibcode:2022PhR...988....1S. doi:10.1016/j.physrep.2022.09.001. S2CID 252111027.
[31]
Schmitt, Andreas (2010). Dense Matter in Compact Stars: A Pedagogical Introduction. Lecture Notes in Physics. Vol. 811. Springer. pp. 4, 143. arXiv:1001.3294. doi:10.1007/978-3-642-12866-0. ISBN 978-3-642-12866-0.
[32]
Boss, L. (1910). Preliminary General Catalogue of 6188 stars for the epoch 1900. Carnegie Institution of Washington. Bibcode:1910pgcs.book.....B. LCCN 10009645 – via Archive.org.
[33]
Liebert, James; Young, P. A.; Arnett, D.; Holberg, J. B.; Williams, K. A. (2005). "The age and progenitor mass of Sirius B". The Astrophysical Journal. 630 (1): L69. arXiv:astro-ph/0507523. Bibcode:2005ApJ...630L..69L. doi:10.1086/462419. S2CID 8792889.
[34]
Öpik, E. (1916). "The densities of visual binary stars". The Astrophysical Journal. 44: 292. Bibcode:1916ApJ....44..292O. doi:10.1086/142296.
[35]
Eddington, A.S. (1927). Stars and Atoms. Clarendon Press. LCCN 27015694.
[36]
Adams, W. S. (1925). "The Relativity Displacement of the Spectral Lines in the Companion of Sirius". Proceedings of the National Academy of Sciences. 11 (7): 382–387. Bibcode:1925PNAS...11..382A. doi:10.1073/pnas.11.7.382. PMC 1086032. PMID 16587023.
[37]
Celotti, A.; Miller, J.C.; Sciama, D.W. (1999). "Astrophysical evidence for the existence of black holes". Class. Quantum Grav. 16 (12A): A3 – A21. arXiv:astro-ph/9912186. Bibcode:1999CQGra..16A...3C. doi:10.1088/0264-9381/16/12A/301. S2CID 17677758.
[38]
Nave, C. R. "Nuclear Size and Density". HyperPhysics. Georgia State University. Archived from the original on 6 July 2009. Retrieved 26 June 2009.
[39]
Adams, Steve (1997). Relativity: an introduction to space-time physics. London; Bristol: CRC Press. p. 240. Bibcode:1997rist.book.....A. ISBN 978-0-7484-0621-0.
[40]
Fowler, R. H. (1926). "On dense matter". Monthly Notices of the Royal Astronomical Society. 87 (2): 114–122. Bibcode:1926MNRAS..87..114F. doi:10.1093/mnras/87.2.114.
[41]
Hoddeson, L. H.; Baym, G. (1980). "The Development of the Quantum Mechanical Electron Theory of Metals: 1900–28". Proceedings of the Royal Society of London. 371 (1744): 8–23. Bibcode:1980RSPSA.371....8H. doi:10.1098/rspa.1980.0051. JSTOR 2990270. S2CID 120476662.
[42]
"Estimating Stellar Parameters from Energy Equipartition". ScienceBits. Archived from the original on 22 May 2012. Retrieved 9 May 2007.
[43]
Bean, R. "Lecture 12 – Degeneracy pressure" (PDF). Lecture notes, Astronomy 211. Cornell University. Archived from the original (PDF) on 25 September 2007. Retrieved 21 September 2007.
[44]
Anderson, W. (1929). "Über die Grenzdichte der Materie und der Energie". Zeitschrift für Physik (in German). 56 (11–12): 851–856. Bibcode:1929ZPhy...56..851A. doi:10.1007/BF01340146. S2CID 122576829.
[45]
Stoner, C. (1930). "The Equilibrium of Dense Stars". Philosophical Magazine. 9: 944.
[46]
Chandrasekhar, S. (1931). "The Maximum Mass of Ideal White Dwarfs". The Astrophysical Journal. 74: 81. Bibcode:1931ApJ....74...81C. doi:10.1086/143324.
[47]
Chandrasekhar, S. (1935). "The highly collapsed configurations of a stellar mass (Second paper)". Monthly Notices of the Royal Astronomical Society. 95 (3): 207–225. Bibcode:1935MNRAS..95..207C. doi:10.1093/mnras/95.3.207.
[48]
"The Nobel Prize in Physics 1983". The Nobel Foundation. Archived from the original on 6 May 2007. Retrieved 4 May 2007.
[49]
Low, Andrew M. (2023). "The Chandrasekhar limit: a simplified approach". Physics Education. 58 (4): 045008. Bibcode:2023PhyEd..58d5008L. doi:10.1088/1361-6552/acdbb0.
[50]
Canal, R.; Gutierrez, J. (1997). "The Possible White Dwarf-Neutron Star Connection". White Dwarfs. Astrophysics and Space Science Library. Vol. 214. pp. 49–55. arXiv:astro-ph/9701225. Bibcode:1997ASSL..214...49C. doi:10.1007/978-94-011-5542-7_7. ISBN 978-94-010-6334-0. S2CID 9288287.
[51]
Lieb, E. H.; Yau, H.-T. (1987). "A rigorous examination of the Chandrasekhar theory of stellar collapse". The Astrophysical Journal. 323 (1): 140–144. Bibcode:1987ApJ...323..140L. doi:10.1086/165813. Retrieved 20 March 2020.
[52]
Mazzali, P. A.; Röpke, F. K.; Benetti, S.; Hillebrandt, W. (2007). "A Common Explosion Mechanism for Type Ia Supernovae". Science. 315 (5813): 825–828. arXiv:astro-ph/0702351. Bibcode:2007Sci...315..825M. doi:10.1126/science.1136259. PMID 17289993.
[53]
Wheeler, J. C. (2000). Cosmic Catastrophes: Supernovae, Gamma-Ray Bursts, and Adventures in Hyperspace. Cambridge University Press. p. 96. ISBN 978-0-521-65195-0.
[54]
Piro, A. L.; Thompson, T. A.; Kochanek, C. S. (2014). "Reconciling 56Ni production in Type Ia supernovae with double degenerate scenarios". Monthly Notices of the Royal Astronomical Society. 438 (4): 3456. arXiv:1308.0334. Bibcode:2014MNRAS.438.3456P. doi:10.1093/mnras/stt2451. S2CID 27316605.
[55]
Chen, W.-C.; Li, X.-D. (2009). "On the Progenitors of Super-Chandrasekhar Mass Type Ia Supernovae". The Astrophysical Journal. 702 (1): 686–691. arXiv:0907.0057. Bibcode:2009ApJ...702..686C. doi:10.1088/0004-637X/702/1/686. S2CID 14301164.
[56]
Howell, D. A.; Sullivan, M.; Conley, A. J.; Carlberg, R. G. (2007). "Predicted and Observed Evolution in the Mean Properties of Type Ia Supernovae with Redshift". Astrophysical Journal Letters. 667 (1): L37 – L40. arXiv:astro-ph/0701912. Bibcode:2007ApJ...667L..37H. doi:10.1086/522030. S2CID 16667595.
[57]
Coelho, Rodrigo C. V.; Calvão, Maurício O.; Reis, Ribamar R. R.; Siffert, Beatriz B. (2015). "Standardization of type Ia supernovae". European Journal of Physics. 36 (1): 015007. arXiv:1411.3596. Bibcode:2015EJPh...36a5007C. doi:10.1088/0143-0807/36/1/015007.
[58]
Chabrier, G.; Baraffe, I. (2000). "Theory of low-Mass stars and substellar objects". Annual Review of Astronomy and Astrophysics. 38: 337–377. arXiv:astro-ph/0006383. Bibcode:2000ARA&A..38..337C. doi:10.1146/annurev.astro.38.1.337. S2CID 59325115.
[59]
Kaler, J. "The Hertzsprung-Russell (HR) diagram". Archived from the original on 31 August 2009. Retrieved 5 May 2007.
[60]
"Basic symbols". Standards for Astronomical Catalogues, Version 2.0. VizieR. Archived from the original on 8 May 2017. Retrieved 12 January 2007.
[61]
Tohline, J. E. "The Structure, Stability, and Dynamics of Self-Gravitating Systems". Archived from the original on 27 June 2010. Retrieved 30 May 2007.
[62]
Hoyle, F. (1947). "Stars, Distribution and Motions of, Note on equilibrium configurations for rotating white dwarfs". Monthly Notices of the Royal Astronomical Society. 107 (2): 231–236. Bibcode:1947MNRAS.107..231H. doi:10.1093/mnras/107.2.231.
[63]
Ostriker, J. P.; Bodenheimer, P. (1968). "Rapidly Rotating Stars. II. Massive White Dwarfs". The Astrophysical Journal. 151: 1089. Bibcode:1968ApJ...151.1089O. doi:10.1086/149507.
[64]
Chanillo, Sagun; Li, Yan Yan (1994). "On diameters of uniformly rotating stars". Communications in Mathematical Physics. 166 (2): 417. Bibcode:1994CMaPh.166..417C. doi:10.1007/BF02112323. S2CID 8372549.
[65]
Chanillo, Sagun; Weiss, Georg S. (2012). "A remark on the geometry of uniformly rotating stars". Journal of Differential Equations. 253 (2): 553. arXiv:1109.3046. Bibcode:2012JDE...253..553C. doi:10.1016/j.jde.2012.04.011. S2CID 144301.
[66]
Sion, E. M.; Greenstein, J. L.; Landstreet, J. D.; Liebert, James; Shipman, H. L.; Wegner, G. A. (1983). "A proposed new white dwarf spectral classification system". The Astrophysical Journal. 269: 253. Bibcode:1983ApJ...269..253S. doi:10.1086/161036.
[67]
Hambly, N. C.; Smartt, S. J.; Hodgkin, S. T. (1997). "WD 0346+246: A Very Low Luminosity, Cool Degenerate in Taurus". The Astrophysical Journal. 489 (2): L157. Bibcode:1997ApJ...489L.157H. doi:10.1086/316797.
[68]
Fontaine, G.; Wesemael, F. (2001). "White dwarfs". In Murdin, P. (ed.). Encyclopedia of Astronomy and Astrophysics. IOP Publishing/Nature Publishing Group. ISBN 978-0-333-75088-9.
[69]
Heise, J. (1985). "X-ray emission from isolated hot white dwarfs". Space Science Reviews. 40 (1–2): 79–90. Bibcode:1985SSRv...40...79H. doi:10.1007/BF00212870. S2CID 120431159.
[70]
Lesaffre, P.; Podsiadlowski, Ph.; Tout, C. A. (2005). "A two-stream formalism for the convective Urca process". Monthly Notices of the Royal Astronomical Society. 356 (1): 131–144. arXiv:astro-ph/0411016. Bibcode:2005MNRAS.356..131L. doi:10.1111/j.1365-2966.2004.08428.x. S2CID 15797437.
[71]
Mestel, L. (1952). "On the theory of white dwarf stars. I. The energy sources of white dwarfs". Monthly Notices of the Royal Astronomical Society. 112 (6): 583–597. Bibcode:1952MNRAS.112..583M. doi:10.1093/mnras/112.6.583.
[72]
Kawaler, S. D. (1998). White Dwarf Stars and the Hubble Deep Field. The Hubble Deep Field: Proceedings of the Space Telescope Science Institute Symposium. p. 252. arXiv:astro-ph/9802217. Bibcode:1998hdf..symp..252K. ISBN 978-0-521-63097-9.
[73]
Bergeron, P.; Ruiz, M. T.; Leggett, S. K. (1997). "The Chemical Evolution of Cool White Dwarfs and the Age of the Local Galactic Disk". The Astrophysical Journal Supplement Series. 108 (1): 339–387. Bibcode:1997ApJS..108..339B. doi:10.1086/312955.
[74]
McCook, G. P.; Sion, E. M. (1999). "A Catalogue of Spectroscopically Identified White Dwarfs". The Astrophysical Journal Supplement Series. 121 (1): 1–130. Bibcode:1999ApJS..121....1M. doi:10.1086/313186.
[75]
Leggett, S. K.; Ruiz, M. T.; Bergeron, P. (1998). "The Cool White Dwarf Luminosity Function and the Age of the Galactic Disk". The Astrophysical Journal. 497 (1): 294–302. Bibcode:1998ApJ...497..294L. doi:10.1086/305463.
[76]
Gates, E.; Gyuk, G.; Harris, H. C.; Subbarao, M.; Anderson, S.; Kleinman, S. J.; et al. (2004). "Discovery of New Ultracool White Dwarfs in the Sloan Digital Sky Survey". The Astrophysical Journal. 612 (2): L129. arXiv:astro-ph/0405566. Bibcode:2004ApJ...612L.129G. doi:10.1086/424568. S2CID 7570539.
[77]
Elms, Abbigail K.; Tremblay, Pier-Emmanuel; Gänsicke, Boris T.; Koester, Detlev; Hollands, Mark A.; Gentile Fusillo, Nicola Pietro; Cunningham, Tim; Apps, Kevin (1 December 2022). "Spectral analysis of ultra-cool white dwarfs polluted by planetary debris". Monthly Notices of the Royal Astronomical Society. 517 (3): 4557–4574. arXiv:2206.05258. Bibcode:2022MNRAS.517.4557E. doi:10.1093/mnras/stac2908. ISSN 0035-8711.
[78]
Winget, D. E.; Hansen, C. J.; Liebert, James; Van Horn, H. M.; Fontaine, G.; Nather, R. E.; Kepler, S. O.; Lamb, D. Q. (1987). "An independent method for determining the age of the universe". The Astrophysical Journal. 315: L77. Bibcode:1987ApJ...315L..77W. doi:10.1086/184864. hdl:10183/108730.
[79]
Trefil, J. S. (2004). The Moment of Creation: Big Bang Physics from Before the First Millisecond to the Present Universe. Dover Publications. ISBN 978-0-486-43813-9.
[80]
Bergeron, P.; Kilic, Mukremin; Blouin, Simon; Bédard, A.; Leggett, S. K.; Brown, Warren R. (1 July 2022). "On the Nature of Ultracool White Dwarfs: Not so Cool after All". The Astrophysical Journal. 934 (1): 36. arXiv:2206.03174. Bibcode:2022ApJ...934...36B. doi:10.3847/1538-4357/ac76c7. ISSN 0004-637X.
[81]
van Horn, H. M. (January 1968). "Crystallization of White Dwarfs". The Astrophysical Journal. 151: 227. Bibcode:1968ApJ...151..227V. doi:10.1086/149432.
[82]
Barrat, J. L.; Hansen, J. P.; Mochkovitch, R. (1988). "Crystallization of carbon-oxygen mixtures in white dwarfs". Astronomy and Astrophysics. 199 (1–2): L15. Bibcode:1988A&A...199L..15B.
[83]
Winget, D. E. (1995). "The Status of White Dwarf Asteroseismology and a Glimpse of the Road Ahead". Baltic Astronomy. 4 (2): 129. Bibcode:1995BaltA...4..129W. doi:10.1515/astro-1995-0209.
[84]
Metcalfe, T. S.; Montgomery, M. H.; Kanaan, A. (20 April 2004). "Testing White Dwarf Crystallization Theory with Asteroseismology of the Massive Pulsating DA Star BPM 37093". The Astrophysical Journal. 605 (2): L133 – L136. arXiv:astro-ph/0402046. Bibcode:2004ApJ...605L.133M. doi:10.1086/420884. S2CID 119378552.
[85]
Whitehouse, David (16 February 2004). "Diamond star thrills astronomers". BBC News. Archived from the original on 5 February 2007. Retrieved 6 January 2007.
[86]
Kanaan, A.; Nitta, A.; Winget, D. E.; Kepler, S. O.; Montgomery, M. H.; Metcalfe, T. S.; et al. (2005). "Whole Earth Telescope observations of BPM 37093: A seismological test of crystallization theory in white dwarfs". Astronomy and Astrophysics. 432 (1): 219–224. arXiv:astro-ph/0411199. Bibcode:2005A&A...432..219K. doi:10.1051/0004-6361:20041125. S2CID 7297628.
[87]
Brassard, P.; Fontaine, G. (2005). "Asteroseismology of the Crystallized ZZ Ceti Star BPM 37093: A Different View". The Astrophysical Journal. 622 (1): 572–576. Bibcode:2005ApJ...622..572B. doi:10.1086/428116.
[88]
Hansen, B. M. S.; Liebert, James (2003). "Cool White Dwarfs". Annual Review of Astronomy and Astrophysics. 41: 465. Bibcode:2003ARA&A..41..465H. doi:10.1146/annurev.astro.41.081401.155117.
[89]
Antoine, Bédard; Simon, Blouin; Sihao, Cheng (2024). "Buoyant crystals halt the cooling of white dwarf stars". Nature. 627 (8003): 286–288. arXiv:2409.04419. Bibcode:2024Natur.627..286B. doi:10.1038/s41586-024-07102-y. ISSN 1476-4687. PMID 38448597.
[90]
Althaus, L. G.; García-Berro, E.; Isern, J.; Córsico, A. H.; Miller Bertolami, M. M. (January 2012). "New phase diagrams for dense carbon-oxygen mixtures and white dwarf evolution". Astronomy & Astrophysics. 537: A33. arXiv:1110.5665. Bibcode:2012A&A...537A..33A. doi:10.1051/0004-6361/201117902. S2CID 119279832.
[91]
Blouin, Simon; Daligault, Jérôme; Saumon, Didier (1 April 2021). "22 Ne Phase Separation as a Solution to the Ultramassive White Dwarf Cooling Anomaly". The Astrophysical Journal Letters. 911 (1): L5. arXiv:2103.12892. Bibcode:2021ApJ...911L...5B. doi:10.3847/2041-8213/abf14b. S2CID 232335433.
[92]
Blouin, Simon; Daligault, Jérôme; Saumon, Didier; Bédard, Antoine; Brassard, Pierre (August 2020). "Toward precision cosmochronology: A new C/O phase diagram for white dwarfs". Astronomy & Astrophysics. 640: L11. arXiv:2007.13669. Bibcode:2020A&A...640L..11B. doi:10.1051/0004-6361/202038879. S2CID 220793255.
[93]
Tremblay, P.-E.; Fontaine, G.; Fusillo, N. P. G.; Dunlap, B. H.; Gänsicke, B. T.; Hollands, M. H.; et al. (2019). "Core crystallization and pile-up in the cooling sequence of evolving white dwarfs" (PDF). Nature. 565 (7738): 202–205. arXiv:1908.00370. Bibcode:2019Natur.565..202T. doi:10.1038/s41586-018-0791-x. PMID 30626942. S2CID 58004893. Archived (PDF) from the original on 23 July 2019. Retrieved 23 July 2019.
[94]
Chen, J.; et al. (2021). "Slowly cooling white dwarfs in M13 from stable hydrogen burning". Nature Astronomy. 5 (11): 1170–1177. arXiv:2109.02306. Bibcode:2021NatAs...5.1170C. doi:10.1038/s41550-021-01445-6.
[95]
Istrate, A. G.; Tauris, T. M.; Langer, N.; Antoniadis, J. (2014). "The timescale of low-mass proto-helium white dwarf evolution". Astronomy and Astrophysics. 571: L3. arXiv:1410.5471. Bibcode:2014A&A...571L...3I. doi:10.1051/0004-6361/201424681. S2CID 55152203.
[96]
"First Giant Planet around White Dwarf Found – ESO observations indicate the Neptune-like exoplanet is evaporating". www.eso.org. Archived from the original on 4 December 2019. Retrieved 4 December 2019.
[97]
Schatzman, E. (1945). "Théorie du débit d'énergie des naines blanches". Annales d'Astrophysique. 8: 143. Bibcode:1945AnAp....8..143S.
[98]
Koester, D.; Chanmugam, G. (1990). "Physics of white dwarf stars". Reports on Progress in Physics. 53 (7): 837–915. Bibcode:1990RPPh...53..837K. doi:10.1088/0034-4885/53/7/001. S2CID 122582479.
[99]
Kawaler, S. D. (1997). "White Dwarf Stars". In Kawaler, S. D.; Novikov, I.; Srinivasan, G. (eds.). Stellar remnants. 1997. ISBN 978-3-540-61520-0.
[100]
Kuiper, G. P. (1941). "List of Known White Dwarfs". Publications of the Astronomical Society of the Pacific. 53 (314): 248. Bibcode:1941PASP...53..248K. doi:10.1086/125335.
[101]
Luyten, W. J. (1952). "The Spectra and Luminosities of White Dwarfs". The Astrophysical Journal. 116: 283. Bibcode:1952ApJ...116..283L. doi:10.1086/145612.
[102]
Greenstein, J. L. (1960). Stellar atmospheres. University of Chicago Press. Bibcode:1960stat.book.....G. LCCN 61-9138.
[103]
Kepler, S. O.; Kleinman, S. J.; Nitta, A.; Koester, D.; Castanheira, B. G.; Giovannini, O.; Costa, A. F. M.; Althaus, L. (2007). "White dwarf mass distribution in the SDSS". Monthly Notices of the Royal Astronomical Society. 375 (4): 1315–1324. arXiv:astro-ph/0612277. Bibcode:2007MNRAS.375.1315K. doi:10.1111/j.1365-2966.2006.11388.x. S2CID 10892288.
[104]
Dufour, P.; Liebert, James; Fontaine, G.; Behara, N. (2007). "White dwarf stars with carbon atmospheres". Nature. 450 (7169): 522–4. arXiv:0711.3227. Bibcode:2007Natur.450..522D. doi:10.1038/nature06318. PMID 18033290. S2CID 4398697.
[105]
Xu, S.; Jura, M.; Koester, D.; Klein, B.; Zuckerman, B. (2013). "Discovery of Molecular Hydrogen in White Dwarf Atmospheres". The Astrophysical Journal. 766 (2): L18. arXiv:1302.6619. Bibcode:2013ApJ...766L..18X. doi:10.1088/2041-8205/766/2/L18. S2CID 119248244.
[106]
Weisskopf, Martin C.; Wu, Kinwah; Trimble, Virginia; O’Dell, Stephen L.; Elsner, Ronald F.; Zavlin, Vyacheslav E.; Kouveliotou, Chryssa (10 March 2007). "A Chandra Search for Coronal X-Rays from the Cool White Dwarf GD 356". The Astrophysical Journal. 657 (2): 1026–1036. arXiv:astro-ph/0609585. Bibcode:2007ApJ...657.1026W. doi:10.1086/510776. ISSN 0004-637X.
[107]
Route, Matthew (20 December 2024). "The Decline and Fall of ROME. V. A Preliminary Search for Star-disrupted Planet Interactions and Coronal Activity at 5 GHz among White Dwarfs within 25 pc". The Astrophysical Journal. 977 (1): 261. arXiv:2411.13718. Bibcode:2024ApJ...977..261R. doi:10.3847/1538-4357/ad9567.
[108]
Jura, M.; Young, E.D. (1 January 2014). "Extrasolar Cosmochemistry". Annual Review of Earth and Planetary Sciences. 42 (1): 45–67. Bibcode:2014AREPS..42...45J. doi:10.1146/annurev-earth-060313-054740.
[109]
Wilson, D.J.; Gänsicke, B.T.; Koester, D.; Toloza, O.; Pala, A. F.; Breedt, E.; Parsons, S.G. (11 August 2015). "The composition of a disrupted extrasolar planetesimal at SDSS J0845+2257 (Ton 345)". Monthly Notices of the Royal Astronomical Society. 451 (3): 3237–3248. arXiv:1505.07466. Bibcode:2015MNRAS.451.3237W. doi:10.1093/mnras/stv1201. S2CID 54049842.
[110]
Blackett, P. M. S. (1947). "The Magnetic Field of Massive Rotating Bodies". Nature. 159 (4046): 658–66. Bibcode:1947Natur.159..658B. doi:10.1038/159658a0. PMID 20239729. S2CID 4133416.
[111]
Lovell, B. (1975). "Patrick Maynard Stuart Blackett, Baron Blackett, of Chelsea. 18 November 1897 – 13 July 1974". Biographical Memoirs of Fellows of the Royal Society. 21: 1–115. doi:10.1098/rsbm.1975.0001. JSTOR 769678. S2CID 74674634.
[112]
Landstreet, John D. (1967). "Synchrotron radiation of neutrinos and its astrophysical significance". Physical Review. 153 (5): 1372–1377. Bibcode:1967PhRv..153.1372L. doi:10.1103/PhysRev.153.1372.
[113]
Ginzburg, V. L.; Zheleznyakov, V. V.; Zaitsev, V. V. (1969). "Coherent mechanisms of radio emission and magnetic models of pulsars". Astrophysics and Space Science. 4 (4): 464–504. Bibcode:1969Ap&SS...4..464G. doi:10.1007/BF00651351. S2CID 119003761.
[114]
Kemp, J.C.; Swedlund, J.B.; Landstreet, J.D.; Angel, J.R.P. (1970). "Discovery of circularly polarized light from a white dwarf". The Astrophysical Journal. 161: L77. Bibcode:1970ApJ...161L..77K. doi:10.1086/180574.
[115]
Ferrario, Lilia; de Martino, Domtilla; Gaensicke, Boris (2015). "Magnetic white dwarfs". Space Science Reviews. 191 (1–4): 111–169. arXiv:1504.08072. Bibcode:2015SSRv..191..111F. doi:10.1007/s11214-015-0152-0. S2CID 119057870.
[116]
Kepler, S.O.; Pelisoli, I.; Jordan, S.; Kleinman, S.J.; Koester, D.; Kuelebi, B.; Pecanha, V.; Castanhiera, B.G.; Nitta, A.; Costa, J.E.S.; Winget, D.E.; Kanaan, A.; Fraga, L. (2013). "Magnetic white dwarf stars in the Sloan Digital Sky Survey". Monthly Notices of the Royal Astronomical Society. 429 (4): 2934–2944. arXiv:1211.5709. Bibcode:2013MNRAS.429.2934K. doi:10.1093/mnras/sts522. S2CID 53316287.
[117]
Landstreet, J.D.; Bagnulo, S.; Valyavin, G.G.; Fossati, L.; Jordan, S.; Monin, D.; Wade, G.A. (2012). "On the incidence of weak magnetic fields in DA white dwarfs". Astronomy and Astrophysics. 545 (A30): 9pp. arXiv:1208.3650. Bibcode:2012A&A...545A..30L. doi:10.1051/0004-6361/201219829. S2CID 55153825.
[118]
Liebert, James; Bergeron, P.; Holberg, J. B. (2003). "The True Incidence of Magnetism Among Field White Dwarfs". The Astronomical Journal. 125 (1): 348–353. arXiv:astro-ph/0210319. Bibcode:2003AJ....125..348L. doi:10.1086/345573. S2CID 9005227.
[119]
Merali, Zeeya (19 July 2012). "Stars draw atoms closer together". Nature News & Comment. Nature. doi:10.1038/nature.2012.11045. Archived from the original on 20 July 2012. Retrieved 21 July 2012.
[120]
Buckley, D.A.H.; Meintjes, P.J.; Potter, S.B.; Marsh, T.R.; Gänsicke, B.T. (23 January 2017). "Polarimetric evidence of a white dwarf pulsar in the binary system AR Scorpii". Nature Astronomy. 1 (2): 0029. arXiv:1612.03185. Bibcode:2017NatAs...1E..29B. doi:10.1038/s41550-016-0029. S2CID 15683792.
[121]
Pelisoli, Ingrid; et al. (2023). "A 5.3-min-period pulsing white dwarf in a binary detected from radio to X-rays". Nature Astronomy. 7 (8): 931–942. arXiv:2306.09272. Bibcode:2023NatAs...7..931P. doi:10.1038/s41550-023-01995-x.
[122]
"ZZ Ceti variables". Centre deDonnées astronomiques de Strasbourg. Association Française des Observateurs d'Etoiles Variables. Archived from the original on 5 February 2007. Retrieved 6 June 2007.
[123]
Quirion, P.-O.; Fontaine, G.; Brassard, P. (2007). "Mapping the Instability Domains of GW Vir Stars in the Effective Temperature–Surface Gravity Diagram". The Astrophysical Journal Supplement Series. 171 (1): 219–248. Bibcode:2007ApJS..171..219Q. doi:10.1086/513870.
[124]
Lawrence, G. M.; Ostriker, J. P.; Hesser, J. E. (1967). "Ultrashort-Period Stellar Oscillations. I. Results from White Dwarfs, Old Novae, Central Stars of Planetary Nebulae, 3c 273, and Scorpius XR-1". The Astrophysical Journal. 148: L161. Bibcode:1967ApJ...148L.161L. doi:10.1086/180037.
[125]
Landolt, A. U. (1968). "A New Short-Period Blue Variable". The Astrophysical Journal. 153: 151. Bibcode:1968ApJ...153..151L. doi:10.1086/149645.
[126]
Nagel, T.; Werner, K. (2004). "Detection of non-radial g-mode pulsations in the newly discovered PG 1159 star HE 1429-1209". Astronomy and Astrophysics. 426 (2): L45. arXiv:astro-ph/0409243. Bibcode:2004A&A...426L..45N. doi:10.1051/0004-6361:200400079. S2CID 9481357.
[127]
O'Brien, M. S. (2000). "The Extent and Cause of the Pre–White Dwarf Instability Strip". The Astrophysical Journal. 532 (2): 1078–1088. arXiv:astro-ph/9910495. Bibcode:2000ApJ...532.1078O. doi:10.1086/308613. S2CID 115958740.
[128]
Winget, D. E. (1998). "Asteroseismology of white dwarf stars". Journal of Physics: Condensed Matter. 10 (49): 11247–11261. Bibcode:1998JPCM...1011247W. doi:10.1088/0953-8984/10/49/014. S2CID 250749380.
[129]
Heger, A.; Fryer, C. L.; Woosley, S. E.; Langer, N.; Hartmann, D. H. (2003). "How Massive Single Stars End Their Life". The Astrophysical Journal. 591 (1): 288–300. arXiv:astro-ph/0212469. Bibcode:2003ApJ...591..288H. doi:10.1086/375341. S2CID 59065632.
[130]
Napiwotzki, Ralf (2009). "The galactic population of white dwarfs". Journal of Physics. Conference Series. 172 (1): 012004. arXiv:0903.2159. Bibcode:2009JPhCS.172a2004N. doi:10.1088/1742-6596/172/1/012004. S2CID 17521113.
[131]
Brown, J. M.; Kilic, M.; Brown, W. R.; Kenyon, S. J. (2011). "The binary fraction of low-mass white dwarfs". The Astrophysical Journal. 730 (67): 67. arXiv:1101.5169. Bibcode:2011ApJ...730...67B. doi:10.1088/0004-637X/730/2/67.
[132]
Laughlin, G.; Bodenheimer, P.; Adams, Fred C. (1997). "The End of the Main Sequence". The Astrophysical Journal. 482 (1): 420–432. Bibcode:1997ApJ...482..420L. doi:10.1086/304125.
[133]
Jeffery, Simon. "Stars Beyond Maturity". Archived from the original on 4 April 2015. Retrieved 3 May 2007.
[134]
Sarna, M. J.; Ergma, E.; Gerškevitš, J. (2001). "Helium core white dwarf evolution – including white dwarf companions to neutron stars". Astronomische Nachrichten. 322 (5–6): 405–410. Bibcode:2001AN....322..405S. doi:10.1002/1521-3994(200112)322:5/6<405::AID-ASNA405>3.0.CO;2-6.
[135]
Benvenuto, O. G.; De Vito, M. A. (2005). "The formation of helium white dwarfs in close binary systems – II". Monthly Notices of the Royal Astronomical Society. 362 (3): 891–905. Bibcode:2005MNRAS.362..891B. doi:10.1111/j.1365-2966.2005.09315.x.
[136]
Nelemans, G.; Tauris, T. M. (1998). "Formation of undermassive single white dwarfs and the influence of planets on late stellar evolution". Astronomy and Astrophysics. 335: L85. arXiv:astro-ph/9806011. Bibcode:1998A&A...335L..85N.
[137]
Zhang, Xianfei; Hall, Philip D.; Jeffery, C. Simon; Bi, Shaolan (2018). "Evolution models of helium white dwarf–main-sequence star merger remnants: the mass distribution of single low-mass white dwarfs". Monthly Notices of the Royal Astronomical Society. 474: 427–432. arXiv:1711.03285. doi:10.1093/mnras/stx2747.
[138]
Woosley, S. E.; Heger, A.; Weaver, T. A. (2002). "The evolution and explosion of massive stars". Reviews of Modern Physics. 74 (4): 1015–1071. Bibcode:2002RvMP...74.1015W. doi:10.1103/RevModPhys.74.1015.
[139]
Dhillon, Vik. "The evolution of low-mass stars". lecture notes, Physics 213. University of Sheffield. Archived from the original on 7 November 2012. Retrieved 3 May 2007.
[140]
Dhillon, Vik. "The evolution of high-mass stars". lecture notes, Physics 213. University of Sheffield. Archived from the original on 7 November 2012. Retrieved 3 May 2007.
[141]
Schaffner-Bielich, Jürgen (2005). "Strange quark matter in stars: A general overview". Journal of Physics G: Nuclear and Particle Physics. 31 (6): S651 – S657. arXiv:astro-ph/0412215. Bibcode:2005JPhG...31S.651S. doi:10.1088/0954-3899/31/6/004. S2CID 118886040.
[142]
Nomoto, K. (1984). "Evolution of 8–10 solar mass stars toward electron capture supernovae. I – Formation of electron-degenerate O + NE + MG cores". The Astrophysical Journal. 277: 791. Bibcode:1984ApJ...277..791N. doi:10.1086/161749.
[143]
Werner, K.; Rauch, T.; Barstow, M. A.; Kruk, J. W. (2004). "Chandra and FUSE spectroscopy of the hot bare stellar core H?1504+65". Astronomy and Astrophysics. 421 (3): 1169–1183. arXiv:astro-ph/0404325. Bibcode:2004A&A...421.1169W. doi:10.1051/0004-6361:20047154. S2CID 2983893.
[144]
Livio, Mario; Truran, James W. (1994). "On the interpretation and implications of nova abundances: An abundance of riches or an overabundance of enrichments". The Astrophysical Journal. 425: 797. Bibcode:1994ApJ...425..797L. doi:10.1086/174024.
[145]
Jordan, George C. IV.; Perets, Hagai B.; Fisher, Robert T.; van Rossum, Daniel R. (2012). "Failed-detonation Supernovae: Subluminous Low-velocity Ia Supernovae and their Kicked Remnant White Dwarfs with Iron-rich Cores". The Astrophysical Journal Letters. 761 (2): L23. arXiv:1208.5069. Bibcode:2012ApJ...761L..23J. doi:10.1088/2041-8205/761/2/L23. S2CID 119203015.
[146]
Panei, J. A.; Althaus, L. G.; Benvenuto, O. G. (2000). "The evolution of iron-core white dwarfs". Monthly Notices of the Royal Astronomical Society. 312 (3): 531–539. arXiv:astro-ph/9911371. Bibcode:2000MNRAS.312..531P. doi:10.1046/j.1365-8711.2000.03236.x. S2CID 17854858.
[147]
Adams, Fred C.; Laughlin, Gregory (1997). "A dying universe: The long-term fate and evolution of astrophysical objects". Reviews of Modern Physics. 69 (2): 337–372. arXiv:astro-ph/9701131. Bibcode:1997RvMP...69..337A. doi:10.1103/RevModPhys.69.337. S2CID 12173790.
[148]
Seager, S.; Kuchner, M.; Hier-Majumder, C.; Militzer, B. (19 July 2007). "Mass-Radius Relationships for Solid Exoplanets". The Astrophysical Journal. 669 (2) (published November 2007): 1279–1297. arXiv:0707.2895. Bibcode:2007ApJ...669.1279S. doi:10.1086/521346. S2CID 8369390.
[149]
Bailes, M.; et al. (2011). "Transformation of a Star into a Planet in a Millisecond Pulsar Binary". Science. 333 (6050): 1717–1720. arXiv:1108.5201. Bibcode:2011Sci...333.1717B. doi:10.1126/science.1208890. PMID 21868629.
[150]
Lemonick, Michael (26 August 2011). "Scientists Discover a Diamond as Big as a Planet". Time Magazine. Archived from the original on 24 August 2013. Retrieved 18 June 2015.
[151]
"Hubble finds dead stars "polluted" with planetary debris". ESA/Hubble Press Release. Archived from the original on 9 June 2013. Retrieved 10 May 2013.
[152]
"Comet falling into white dwarf (artist's impression)". www.spacetelescope.org. Archived from the original on 15 February 2017. Retrieved 14 February 2017.
[153]
Koester, D.; Gänsicke, B. T.; Farihi, J. (1 June 2014). "The frequency of planetary debris around young white dwarfs". Astronomy and Astrophysics. 566: A34. arXiv:1404.2617. Bibcode:2014A&A...566A..34K. doi:10.1051/0004-6361/201423691. ISSN 0004-6361. S2CID 119268896.
[154]
Jura, M. (1 May 2008). "Pollution of Single White Dwarfs by Accretion of Many Small Asteroids". The Astronomical Journal. 135 (5): 1785–1792. arXiv:0802.4075. Bibcode:2008AJ....135.1785J. doi:10.1088/0004-6256/135/5/1785. ISSN 0004-6256. S2CID 16571761.
[155]
Debes, John H.; Thévenot, Melina; Kuchner, Marc J.; Burgasser, Adam J.; Schneider, Adam C.; Meisner, Aaron M.; Gagné, Jonathan; Faherty, Jacqueline K.; Rees, Jon M. (19 February 2019). "A 3 Gyr White Dwarf with Warm Dust Discovered via the Backyard Worlds: Planet 9 Citizen Science Project". The Astrophysical Journal. 872 (2): L25. arXiv:1902.07073. Bibcode:2019ApJ...872L..25D. doi:10.3847/2041-8213/ab0426. ISSN 2041-8213. S2CID 119359995.
[156]
van Maanen, A. (1 December 1917). "Two Faint Stars with Large Proper Motion". Publications of the Astronomical Society of the Pacific. 29 (172): 258. Bibcode:1917PASP...29..258V. doi:10.1086/122654. ISSN 0004-6280. S2CID 250734202.
[157]
Klein, Beth L.; Doyle, Alexandra E.; Zuckerman, B.; Dufour, P.; Blouin, Simon; Melis, Carl; Weinberger, Alycia J.; Young, Edward D. (1 June 2021). "Discovery of Beryllium in White Dwarfs Polluted by Planetesimal Accretion". The Astrophysical Journal. 914 (1): 61. arXiv:2102.01834. Bibcode:2021ApJ...914...61K. doi:10.3847/1538-4357/abe40b. ISSN 0004-637X. S2CID 231786441.
[158]
Zuckerman, B. (1 June 2015). Recognition of the First Observational Evidence of an Extrasolar Planetary System. 19Th European Workshop on White Dwarfs. Vol. 493. p. 291. Bibcode:2015ASPC..493..291Z.
[159]
Farihi, J. (1 April 2016). "Circumstellar debris and pollution at white dwarf stars". New Astronomy Reviews. 71: 9–34. arXiv:1604.03092. Bibcode:2016NewAR..71....9F. doi:10.1016/j.newar.2016.03.001. ISSN 1387-6473. S2CID 118486264.
[160]
Zuckerman, B.; Becklin, E. E. (1 November 1987). "Excess infrared radiation from a white dwarf—an orbiting brown dwarf?". Nature. 330 (6144): 138–140. Bibcode:1987Natur.330..138Z. doi:10.1038/330138a0. ISSN 0028-0836. S2CID 4357883.
[161]
Reach, William T.; Kuchner, Marc J.; Von Hippel, Ted; Burrows, Adam; Mullally, Fergal; Kilic, Mukremin; Winget, D. E. (2005). "The Dust Cloud around the White Dwarf G29-38". The Astrophysical Journal. 635 (2): L161. arXiv:astro-ph/0511358. Bibcode:2005ApJ...635L.161R. doi:10.1086/499561. S2CID 119462589.
[162]
Steckloff, Jordan K.; Debes, John; Steele, Amy; Johnson, Brandon; Adams, Elisabeth R.; Jacobson, Seth A.; Springmann, Alessondra (1 June 2021). "How Sublimation Delays the Onset of Dusty Debris Disk Formation around White Dwarf Stars". The Astrophysical Journal. 913 (2): L31. arXiv:2104.14035. Bibcode:2021ApJ...913L..31S. doi:10.3847/2041-8213/abfd39. ISSN 0004-637X. PMC 8740607. PMID 35003618.
[163]
Veras, Dimitri (1 October 2021). "Planetary Systems Around White Dwarfs". Oxford Research Encyclopedia of Planetary Science. Oxford University Press. arXiv:2106.06550. Bibcode:2021orel.bookE...1V. doi:10.1093/acrefore/9780190647926.013.238. ISBN 978-0-19-064792-6.
[164]
Mullally, Susan E.; Debes, John; Cracraft, Misty; Mullally, Fergal; Poulsen, Sabrina; Albert, Loic; Thibault, Katherine; Reach, William T.; Hermes, J. J.; Barclay, Thomas; Kilic, Mukremin; Quintana, Elisa V. (24 January 2024). "JWST Directly Images Giant Planet Candidates Around Two Metal-Polluted White Dwarf Stars". The Astrophysical Journal Letters. 962 (2): L32. arXiv:2401.13153. Bibcode:2024ApJ...962L..32M. doi:10.3847/2041-8213/ad2348.
[165]
"Comet clash kicks up dusty haze". BBC News. 13 February 2007. Archived from the original on 16 February 2007. Retrieved 20 September 2007.
[166]
Su, K. Y. L.; Chu, Y.-H.; Rieke, G. H.; Huggins, P. J.; Gruendl, R.; Napiwotzki, R.; Rauch, T.; Latter, W. B.; Volk, K. (2007). "A Debris Disk around the Central Star of the Helix Nebula?". The Astrophysical Journal. 657 (1): L41. arXiv:astro-ph/0702296. Bibcode:2007ApJ...657L..41S. doi:10.1086/513018. S2CID 15244406.
[167]
Sion, Edward M.; Holberg, J.B.; Oswalt, Terry D.; McCook, George P.; Wasatonic, Richard (2009). "The White Dwarfs Within 20 Parsecs of the Sun: Kinematics and Statistics". The Astronomical Journal. 138 (6): 1681–1689. arXiv:0910.1288. Bibcode:2009AJ....138.1681S. doi:10.1088/0004-6256/138/6/1681. S2CID 119284418.
[168]
Li, Jianke; Ferrario, Lilia; Wickramasinghe, Dayal (1998). "Planets around White Dwarfs". Astrophysical Journal Letters. 503 (1): L151. Bibcode:1998ApJ...503L.151L. doi:10.1086/311546. p. L51.
[169]
Debes, John H.; Walsh, Kevin J.; Stark, Christopher (24 February 2012). "The Link Between Planetary Systems, Dusty White Dwarfs, and Metal-Polluted White Dwarfs". The Astrophysical Journal. 747 (2): 148. arXiv:1201.0756. Bibcode:2012ApJ...747..148D. doi:10.1088/0004-637X/747/2/148. ISSN 0004-637X. S2CID 118688656.
[170]
Veras, Dimitri; Gänsicke, Boris T. (21 February 2015). "Detectable close-in planets around white dwarfs through late unpacking". Monthly Notices of the Royal Astronomical Society. 447 (2): 1049–1058. arXiv:1411.6012. Bibcode:2015MNRAS.447.1049V. doi:10.1093/mnras/stu2475. ISSN 0035-8711. S2CID 119279872.
[171]
Frewen, S. F. N.; Hansen, B. M. S. (11 April 2014). "Eccentric planets and stellar evolution as a cause of polluted white dwarfs". Monthly Notices of the Royal Astronomical Society. 439 (3): 2442–2458. arXiv:1401.5470. Bibcode:2014MNRAS.439.2442F. doi:10.1093/mnras/stu097. ISSN 0035-8711. S2CID 119257046.
[172]
Bonsor, Amy; Gänsicke, Boris T.; Veras, Dimitri; Villaver, Eva; Mustill, Alexander J. (21 May 2018). "Unstable low-mass planetary systems as drivers of white dwarf pollution". Monthly Notices of the Royal Astronomical Society. 476 (3): 3939–3955. arXiv:1711.02940. Bibcode:2018MNRAS.476.3939M. doi:10.1093/mnras/sty446. ISSN 0035-8711. S2CID 4809366.
[173]
Gänsicke, Boris T.; Holman, Matthew J.; Veras, Dimitri; Payne, Matthew J. (21 March 2016). "Liberating exomoons in white dwarf planetary systems". Monthly Notices of the Royal Astronomical Society. 457 (1): 217–231. arXiv:1603.09344. Bibcode:2016MNRAS.457..217P. doi:10.1093/mnras/stv2966. ISSN 0035-8711. S2CID 56091285.
[174]
Rebassa-Mansergas, Alberto; Xu (许偲艺), Siyi; Veras, Dimitri (21 January 2018). "The critical binary star separation for a planetary system origin of white dwarf pollution". Monthly Notices of the Royal Astronomical Society. 473 (3): 2871–2880. arXiv:1708.05391. Bibcode:2018MNRAS.473.2871V. doi:10.1093/mnras/stx2141. ISSN 0035-8711. S2CID 55764122.
[175]
Becklin, E. E.; Zuckerman, B.; Farihi, J. (10 February 2008). "Spitzer IRAC Observations of White Dwarfs. I. Warm Dust at Metal-Rich Degenerates". The Astrophysical Journal. 674 (1): 431–446. arXiv:0710.0907. Bibcode:2008ApJ...674..431F. doi:10.1086/521715. ISSN 0004-637X. S2CID 17813180.
[176]
Lemonick, Michael D. (21 October 2015). "Zombie Star Caught Feasting on Asteroids". National Geographic News. Archived from the original on 24 October 2015. Retrieved 22 October 2015.
[177]
Vanderburg, Andrew; Johnson, John Asher; Rappaport, Saul; Bieryla, Allyson; Irwin, Jonathan; Lewis, John Arban; Kipping, David; Brown, Warren R.; Dufour, Patrick (22 October 2015). "A disintegrating minor planet transiting a white dwarf". Nature. 526 (7574): 546–549. arXiv:1510.06387. Bibcode:2015Natur.526..546V. doi:10.1038/nature15527. PMID 26490620. S2CID 4451207.
[178]
Gänsicke, Boris T.; Schreiber, Matthias R.; Toloza, Odette; Gentile Fusillo, Nicola P.; Koester, Detlev; Manser, Christopher J. "Accretion of a giant planet onto a white dwarf" (PDF). ESO. Archived (PDF) from the original on 4 December 2019. Retrieved 11 December 2019.
[179]
Wang, Ting-Gui; Jiang, Ning; Ge, Jian; Cutri, Roc M.; Jiang, Peng; Sheng, Zhengfeng; Zhou, Hongyan; Bauer, James; Mainzer, Amy; Wright, Edward L. (November 2019). "An On-going Mid-infrared Outburst in the White Dwarf 0145+234: Catching in Action of Tidal Disruption of an Exoasteroid?". Astrophysical Journal Letters. 886 (1): L5. arXiv:1910.04314. Bibcode:2019ApJ...886L...5W. doi:10.3847/2041-8213/ab53ed.
[180]
Vanderburg, Andrew; Rappaport, Saul A.; Xu, Siyi; Crossfield, Ian J. M.; Becker, Juliette C.; Gary, Bruce; et al. (September 2020). "A giant planet candidate transiting a white dwarf". Nature. 585 (7825): 363–367. arXiv:2009.07282. Bibcode:2020Natur.585..363V. doi:10.1038/s41586-020-2713-y. PMID 32939071.
[181]
Kipping, David (January 2024). "The giant nature of WD 1856 b implies that transiting rocky planets are rare around white dwarfs". Monthly Notices of the Royal Astronomical Society. 527 (2): 3532–3541. arXiv:2310.15219. doi:10.1093/mnras/stad3431.
[182]
Blackman, J. W.; Beaulieu, J. P.; Bennett, D. P.; Danielski, C.; Alard, C.; Cole, A. A.; Vandorou, A.; Ranc, C.; Terry, S. K.; Bhattacharya, A.; Bond, I.; Bachelet, E.; Veras, D.; Koshimoto, N.; Batista, V.; Marquette, J. B. (2021). "A Jovian analogue orbiting a white dwarf star". Nature. 598 (7880): 272–275. arXiv:2110.07934. Bibcode:2021Natur.598..272B. doi:10.1038/s41586-021-03869-6. PMID 34646001.
[183]
Kervella, Pierre; Arenou, Frédéric; Mignard, François; Thévenin, Frédéric (1 March 2019). "Stellar and substellar companions of nearby stars from Gaia DR2. Binarity from proper motion anomaly". Astronomy and Astrophysics. 623: A72. arXiv:1811.08902. Bibcode:2019A&A...623A..72K. doi:10.1051/0004-6361/201834371. ISSN 0004-6361. S2CID 119491061.
[184]
Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (1 January 2022). "Stellar and substellar companions from Gaia EDR3. Proper-motion anomaly and resolved common proper-motion pairs". Astronomy and Astrophysics. 657: A7. arXiv:2109.10912. Bibcode:2022A&A...657A...7K. doi:10.1051/0004-6361/202142146. ISSN 0004-6361. S2CID 237605138.
[185]
Gaia Collaboration; Arenou, F.; Babusiaux, C.; Barstow, M. A.; Faigler, S.; Jorissen, A.; Kervella, P.; Mazeh, T.; Mowlavi, N.; Panuzzo, P.; Sahlmann, J.; Shahaf, S.; Sozzetti, A.; Bauchet, N.; Damerdji, Y. (2023). "Gaia Data Release 3". Astronomy & Astrophysics. 674: A34. arXiv:2206.05595. doi:10.1051/0004-6361/202243782. S2CID 249626026.
[186]
"CYCLE 2 GO". STScI.edu. Retrieved 15 May 2023.
[187]
"Gaia DR3 known issues". ESA. 5 May 2023. Retrieved 8 August 2023. During validation of epoch astrometry for Gaia DR4, an error was discovered, that had already had an impact on the Gaia DR3 non-single star results. [...] We can conclude that the solutions for [...] WD 0141-675 [...] are false-positives as far as Gaia non-single star processing is concerned.
[188]
Casewell, S. L.; Debes, J.; Dupuy, T. J.; Dufour, P.; Bonsor, A.; Rebassa-Mansergas, A.; Murillo-Ojeda, R.; French, J. R.; Xu, Siyi (许偲艺); Martin, E.; Manjavacas, E. (8 April 2024). "PHL 5038AB: Is the brown dwarf causing pollution of its white dwarf host star?". MNRAS. 530 (3): 3302–3309. arXiv:2404.05488. doi:10.1093/mnras/stae974.
[189]
Agol, Eric (2011). "Transit Surveys for Earths in the Habitable Zones of White Dwarfs". The Astrophysical Journal Letters. 635 (2): L31. arXiv:1103.2791. Bibcode:2011ApJ...731L..31A. doi:10.1088/2041-8205/731/2/L31. S2CID 118739494.
[190]
Barnes, Rory; Heller, René (2011). "Habitable Planets Around White and Brown Dwarfs: The Perils of a Cooling Primary". Astrobiology. 13 (3): 279–291. arXiv:1211.6467. Bibcode:2013AsBio..13..279B. doi:10.1089/ast.2012.0867. PMC 3612282. PMID 23537137.
[191]
Nordhaus, J.; Spiegel, D.S. (2013). "On the orbits of low-mass companions to white dwarfs and the fates of the known exoplanets". Monthly Notices of the Royal Astronomical Society. 432 (1): 500–505. arXiv:1211.1013. Bibcode:2013MNRAS.432..500N. doi:10.1093/mnras/stt569. S2CID 119227364.
[192]
Di Stefano, R.; Nelson, L. A.; Lee, W.; Wood, T. H.; Rappaport, S. (1997). "Luminous Supersoft X-ray Sources as Type Ia Progenitors". In P. Ruiz-Lapuente; R. Canal; J. Isern (eds.). Thermonuclear Supernovae. NATO Science Series C: Mathematical and physical sciences. Vol. 486. Springer. pp. 148–149. Bibcode:1997ASIC..486..147D. doi:10.1007/978-94-011-5710-0_10. ISBN 978-0-7923-4359-2.
[193]
Lopes de Oliveira, R.; Bruch, A.; Rodrigues, C. V.; de Oliveira, A. S.; Mukai, K. (2020). "CTCV J2056-3014: An X-Ray-faint Intermediate Polar Harboring an Extremely Fast-spinning White Dwarf". The Astrophysical Journal Letters. 898 (2): L40. arXiv:2007.13932. Bibcode:2020ApJ...898L..40L. doi:10.3847/2041-8213/aba618. S2CID 220831174.
[194]
Aguilar, David A.; Pulliam, Christine (16 November 2010). "Astronomers Discover Merging Star Systems that Might Explode". Harvard-Smithsonian Center for Astrophysics. Archived from the original on 9 April 2011. Retrieved 16 February 2011.
[195]
Aguilar, David A.; Pulliam, Christine (13 July 2011). "Evolved Stars Locked in Fatalistic Dance". Harvard-Smithsonian Center for Astrophysics. Archived from the original on 15 July 2011. Retrieved 17 July 2011.
[196]
Yoon, S.-C.; Langer, N. (2004). "Presupernova evolution of accreting white dwarfs with rotation". Astronomy and Astrophysics. 419 (2): 623–644. arXiv:astro-ph/0402287. Bibcode:2004A&A...419..623Y. doi:10.1051/0004-6361:20035822. S2CID 2963085.
[197]
Hillebrandt, W.; Niemeyer, J. C. (2000). "Type IA supernova explosion models". Annual Review of Astronomy and Astrophysics. 38: 191–230. arXiv:astro-ph/0006305. Bibcode:2000ARA&A..38..191H. doi:10.1146/annurev.astro.38.1.191.
[198]
Blinnikov, S. I.; Röpke, F. K.; Sorokina, E. I.; Gieseler, M.; Reinecke, M.; Travaglio, C.; Hillebrandt, W.; Stritzinger, M. (2006). "Theoretical light curves for deflagration models of type Ia supernova". Astronomy and Astrophysics. 453 (1): 229–240. arXiv:astro-ph/0603036. Bibcode:2006A&A...453..229B. doi:10.1051/0004-6361:20054594. S2CID 15493284.
[199]
Maoz, D.; Mannucci, F. (18 January 2012). "Type-Ia Supernova Rates and the Progenitor Problem: A Review". Publications of the Astronomical Society of Australia. 29 (4): 447–465. arXiv:1111.4492. Bibcode:2012PASA...29..447M. doi:10.1071/AS11052. ISSN 1448-6083.
[200]
Wang, Bo; Han, Zhanwen (1 June 2012). "Progenitors of type Ia supernovae". New Astronomy Reviews. 56 (4): 122–141. arXiv:1204.1155. Bibcode:2012NewAR..56..122W. doi:10.1016/j.newar.2012.04.001. ISSN 1387-6473.
[201]
Maoz, Dan; Mannucci, Filippo; Nelemans, Gijs (18 August 2014). "Observational Clues to the Progenitors of Type Ia Supernovae". Annual Review of Astronomy and Astrophysics. 52 (1): 107–170. arXiv:1312.0628. Bibcode:2014ARA&A..52..107M. doi:10.1146/annurev-astro-082812-141031. ISSN 0066-4146.
[202]
González Hernández, J.I.; Ruiz-Lapuente, P.; Tabernero, H. M.; Montes, D.; Canal, R.; Méndez, J.; Bedin, L. R. (2012). "No surviving evolved companions of the progenitor of SN 1006". Nature. 489 (7417): 533–536. arXiv:1210.1948. Bibcode:2012Natur.489..533G. doi:10.1038/nature11447. PMID 23018963. S2CID 4431391.
[203]
Krause, Oliver; et al. (2008). "Tycho Brahe's 1572 supernova as a standard type Ia as revealed by its light-echo spectrum". Nature. 456 (7222): 617–619. arXiv:0810.5106. Bibcode:2008Natur.456..617K. doi:10.1038/nature07608. PMID 19052622. S2CID 4409995.
[204]
de la Fuente Marcos, Raúl; de la Fuente Marcos, Carlos (2022). "Deep and fast Solar System flybys: The controversial case of WD 0810-353". Astronomy & Astrophysics. 668: A14. arXiv:2210.04863. Bibcode:2022A&A...668A..14D. doi:10.1051/0004-6361/202245020. ISSN 0004-6361. S2CID 252863734.
[205]
Landstreet, J. D.; Villaver, E.; Bagnulo, S. (2023). "Not so fast, not so furious: just magnetic". The Astrophysical Journal. 952 (2): 129. arXiv:2306.11663. Bibcode:2023ApJ...952..129L. doi:10.3847/1538-4357/acdac8.
[206]
Kruckow, Matthias U.; Neunteufel, Patrick G.; Di Stefano, Rosanne; Gao, Yan; Kobayashi, Chiaki (2021). "A Catalog of Potential Post–Common Envelope Binaries". The Astrophysical Journal. 920 (2): 86. arXiv:2107.05221. Bibcode:2021ApJ...920...86K. doi:10.3847/1538-4357/ac13ac.
[207]
Nordhaus, J.; Wellons, S.; Spiegel, D. S.; Metzger, B. D.; Blackman, E. G. (2011). "Formation of high-field magnetic white dwarfs from common envelopes". PNAS. 108 (8): 3135–3140. arXiv:1010.1529. Bibcode:2011PNAS..108.3135N. doi:10.1073/pnas.1015005108. PMC 3044383. PMID 21300910.
[208]
Rebassa-Mansergas, A.; Solano, E.; Jiménez-Esteban, F. M.; Torres, S.; Rodrigo, C.; Ferrer-Burjachs, A.; Calcaferro, L. M.; Althaus, L. G.; Córsico, A. H. (October 2021). "White dwarf–main-sequence binaries from Gaia EDR3: the unresolved 100 pc volume-limited sample". Monthly Notices of the Royal Astronomical Society. 506 (4): 5201–5211. arXiv:2107.06303. doi:10.1093/mnras/stab2039.
[209]
Schreiber, M. R.; Gänsicke, B. T. (2003). "The age, life expectancy, and space density of Post Common Envelope Binaries". Astronomy and Astrophysics. 406: 305–321. arXiv:astro-ph/0305531. Bibcode:2003A&A...406..305S. doi:10.1051/0004-6361:20030801.
[210]
"Cataclysmic Variables". fact sheet. Imagine the Universe!. NASA Goddard. Archived from the original on 9 July 2007. Retrieved 4 May 2007.
[211]
"Introduction to Cataclysmic Variables (CVs)". fact sheet. NASA Goddard. Archived from the original on 6 February 2012. Retrieved 4 May 2007.
[212]
Fraknoi, Andrew; et al. (2024). "18.4 The H–R Diagram". Astronomy 2e. OpenStax. p. 618. ISBN 978-1-951693-50-3.
[213]
Perpinyà-Vallès, M.; Rebassa-Mansergas, A.; Gänsicke, B. T.; Toonen, S.; Hermes, J. J.; Gentile Fusillo, N. P.; Tremblay, P.-E. (February 2019). "Discovery of the first resolved triple white dwarf". Monthly Notices of the Royal Astronomical Society. 483 (1): 901–907. arXiv:1811.07752. doi:10.1093/mnras/sty3149.
[214]
Brandner, Wolfgang; Zinnecker, Hans; Kopytova, Taisiya (2021). "Search for giant planets around seven white dwarfs in the Hyades cluster with the Hubble Space Telescope". Monthly Notices of the Royal Astronomical Society. 500 (3): 3920–3925. arXiv:2011.03562. doi:10.1093/mnras/staa3422.
[215]
Luhman, K. L.; Burgasser, A. J.; Bochanski, J. J. (2011). "Discovery of a Candidate for the Coolest Known Brown Dwarf". The Astrophysical Journal Letters. 730 (1): L9. arXiv:1102.5411. Bibcode:2011ApJ...730L...9L. doi:10.1088/2041-8205/730/1/L9.
[216]
Rodriguez, David R.; Zuckerman, B.; Melis, Carl; Song, Inseok (May 2011). "The Ultra Cool Brown Dwarf Companion of WD 0806-661B: Age, Mass, and Formation Mechanism". The Astrophysical Journal Letters. 732 (2): L29. arXiv:1103.3544. Bibcode:2011ApJ...732L..29R. doi:10.1088/2041-8205/732/2/L29.
[217]
Veras, Dimitri; Evans, N. Wyn (21 March 2013). "Exoplanets beyond the Solar neighbourhood: Galactic tidal perturbations". Monthly Notices of the Royal Astronomical Society. 430 (1): 403–415. arXiv:1212.4150. doi:10.1093/mnras/sts647.
[218]
Giammichele, N.; Bergeron, P.; Dufour, P. (April 2012). "Know Your Neighborhood: A Detailed Model Atmosphere Analysis of Nearby White Dwarfs". The Astrophysical Journal Supplement. 199 (2): 35. arXiv:1202.5581. Bibcode:2012ApJS..199...29G. doi:10.1088/0067-0049/199/2/29. S2CID 118304737. 29.
[219]
Delfosse, Xavier; et al. (April 1999). "New neighbours. I. 13 new companions to nearby M dwarfs". Astronomy and Astrophysics. 344: 897–910. arXiv:astro-ph/9812008. Bibcode:1999A&A...344..897D.

General

Kawaler, S. D. (1997). "White Dwarf Stars". In Kawaler, S. D.; Novikov, I.; Srinivasan, G. (eds.). Stellar remnants. 1997. ISBN 978-3-540-61520-0.

Physics

Black holes, white dwarfs, and neutron stars: the physics of compact objects, Stuart L. Shapiro and Saul A. Teukolsky, New York: Wiley, 1983. ISBN 0-471-87317-9.
"Estimating Stellar Parameters from Energy Equipartition". sciencebits.com. — Discusses how to find mass-radius relations and mass limits for white dwarfs using simple energy arguments.

Variability

Winget, D.E. (1998). "Asteroseismology of white dwarf stars". Journal of Physics: Condensed Matter. 10 (49): 11247–11261. Bibcode:1998JPCM...1011247W. doi:10.1088/0953-8984/10/49/014. S2CID 250749380.

Magnetic field

Wickramasinghe, D. T.; Ferrario, Lilia (2000). "Magnetism in Isolated and Binary White Dwarfs". Publications of the Astronomical Society of the Pacific. 112 (773): 873–924. Bibcode:2000PASP..112..873W. doi:10.1086/316593.

Frequency

Gibson, B. K.; Flynn, C (2001). "White Dwarfs and Dark Matter". Science. 292 (5525): 2211a. arXiv:astro-ph/0104255. doi:10.1126/science.292.5525.2211a. PMID 11423620. S2CID 14080941.

Observational

Provencal, J. L.; Shipman, H. L.; Hog, Erik; Thejll, P. (1998). "Testing the White Dwarf Mass-Radius Relation with Hipparcos". The Astrophysical Journal. 494 (2): 759–767. Bibcode:1998ApJ...494..759P. doi:10.1086/305238.
Gates, Evalyn; Gyuk, Geza; Harris, Hugh C.; Subbarao, Mark; Anderson, Scott; Kleinman, S. J.; Liebert, James; Brewington, Howard; et al. (2004). "Discovery of New Ultracool White Dwarfs in the Sloan Digital Sky Survey". The Astrophysical Journal. 612 (2): L129. arXiv:astro-ph/0405566. Bibcode:2004ApJ...612L.129G. doi:10.1086/424568. S2CID 7570539.
McCook, G.P.; Sion, E.M., eds. (9 September 2013). "White Dwarf Catalogue WD". Villanova University. Archived from the original on 6 July 2024.
Dufour, P.; Liebert, James; Fontaine, G.; Behara, N. (2007). "White dwarf stars with carbon atmospheres". Nature. 450 (7169): 522–4. arXiv:0711.3227. Bibcode:2007Natur.450..522D. doi:10.1038/nature06318. PMID 18033290. S2CID 4398697.

Images

White dwarf images at Astronomy Picture of the Day

$\"Featured$ \n"}">

[osln-1] [1]
Johnson, J. (2007). "Extreme stars: White dwarfs & neutron stars" (Lecture notes). Astronomy 162. Ohio State University. Archived from the original on 31 March 2012. Retrieved 17 October 2011.

[2] [2]
Henry, T.J. (1 January 2009). "The one hundred nearest star systems". Research Consortium on Nearby Stars. Archived from the original on 12 November 2007. Retrieved 21 July 2010.

[schatzman-3] [3]
Evry L. Schatzman (1958). White Dwarfs. North-Holland Publishing Company. ISBN 978-0-598-58212-6.

[cosmochronology-4] [4]
Fontaine, G.; Brassard, P.; Bergeron, P. (2001). "The potential of white dwarf cosmochronology". Publications of the Astronomical Society of the Pacific. 113 (782): 409–435. Bibcode:2001PASP..113..409F. doi:10.1086/319535.

[rln-5] [5]
Richmond, M. "Late stages of evolution for low-mass stars". Lecture notes, Physics 230. Rochester Institute of Technology. Archived from the original on 4 September 2017. Retrieved 3 May 2007.

[oxne-6] [6]
Werner, K.; Hammer, N.J.; Nagel, T.; Rauch, T.; Dreizler, S. (2005). On possible oxygen / neon white dwarfs: H1504+65 and the white dwarf donors in ultracompact X-ray binaries. 14th European Workshop on White Dwarfs. Vol. 334. p. 165. arXiv:astro-ph/0410690. Bibcode:2005ASPC..334..165W.

[apj606_L147-7] [7]
Liebert, James; Bergeron, P.; Eisenstein, D.; Harris, H. C.; Kleinman, S. J.; Nitta, A.; Krzesinski, J. (2004). "A helium white dwarf of extremely low mass". The Astrophysical Journal. 606 (2): L147. arXiv:astro-ph/0404291. Bibcode:2004ApJ...606L.147L. doi:10.1086/421462. S2CID 118894713.

[he2-8] [8]
"Cosmic weight loss: The lowest mass white dwarf" (Press release). Harvard-Smithsonian Center for Astrophysics. 17 April 2007. Archived from the original on 22 April 2007. Retrieved 20 April 2007.

[9] [9]
Althaus, L. G.; Benvenuto, O. G. (March 1997). "Evolution of Helium White Dwarfs of Low and Intermediate Masses". The Astrophysical Journal. 477 (1): 313–334. Bibcode:1997ApJ...477..313A. doi:10.1086/303686.

[aou-10] [10]
Spergel, D.N.; Bean, R.; Doré, O.; Nolta, M.R.; Bennett, C.L.; Dunkley, J.; et al. (2007). "Wilkinson Microwave Anisotropy Probe (WMAP) three year results: Implications for cosmology". The Astrophysical Journal Supplement Series. 170 (2): 377–408. arXiv:astro-ph/0603449. Bibcode:2007ApJS..170..377S. doi:10.1086/513700. S2CID 1386346.

[2003ApJ...591..288H-11] [11]
§3, Heger, A.; Fryer, C.L.; Woosley, S.E.; Langer, N.; Hartmann, D.H. (2003). "How massive single stars end their life". Astrophysical Journal. 591 (1): 288–300. arXiv:astro-ph/0212469. Bibcode:2003ApJ...591..288H. doi:10.1086/375341. S2CID 59065632.

[12] [12]
Herschel, W. (1785). "Catalogue of Double Stars". Philosophical Transactions of the Royal Society of London. 75: 40–126. Bibcode:1785RSPT...75...40H. doi:10.1098/rstl.1785.0006. JSTOR 106749. S2CID 186209747.

[holberg-13] [13]
Holberg, J. B. (2005). How degenerate stars came to be known as 'white dwarfs'. American Astronomical Society meeting 207. Vol. 207. p. 1503. Bibcode:2005AAS...20720501H.

[14] [14]
Adams, W.S. (1914). "An A-type star of very low luminosity". Publications of the Astronomical Society of the Pacific. 26 (155): 198. Bibcode:1914PASP...26..198A. doi:10.1086/122337.

[fwbessel-15] [15]
Bessel, F.W. (1844). "On the variations of the proper motions of Procyon and Sirius". Monthly Notices of the Royal Astronomical Society. 6 (11): 136–141. Bibcode:1844MNRAS...6R.136B. doi:10.1093/mnras/6.11.136a.

[flammarion-16] [16]
Flammarion, Camille (1877). "The companion of Sirius". Astronomical Register. 15: 186. Bibcode:1877AReg...15..186F.

[17] [17]
Adams, W.S. (1915). "The spectrum of the companion of Sirius". Publications of the Astronomical Society of the Pacific. 27 (161): 236. Bibcode:1915PASP...27..236A. doi:10.1086/122440.

[18] [18]
van Maanen, A. (1917). "Two faint stars with large proper motion". Publications of the Astronomical Society of the Pacific. 29 (172): 258. Bibcode:1917PASP...29..258V. doi:10.1086/122654.

[19] [19]
Luyten, W.J. (1922). "The mean parallax of early-type stars of determined proper motion and apparent magnitude". Publications of the Astronomical Society of the Pacific. 34 (199): 156. Bibcode:1922PASP...34..156L. doi:10.1086/123176.

[20] [20]
Luyten, W.J. (1922). "Note on some faint early-type stars with large proper motions". Publications of the Astronomical Society of the Pacific. 34 (197): 54. Bibcode:1922PASP...34...54L. doi:10.1086/123146.

[21] [21]
Luyten, W.J. (1922). "Additional note on faint early-type stars with large proper motions". Publications of the Astronomical Society of the Pacific. 34 (198): 132. Bibcode:1922PASP...34..132L. doi:10.1086/123168.

[22] [22]
Aitken, R.G. (1922). "Comet c 1922 (Baade)". Publications of the Astronomical Society of the Pacific. 34 (202): 353. Bibcode:1922PASP...34..353A. doi:10.1086/123244.

[eddington-23] [23]
Eddington, A. S. (1924). "On the relation between the masses and luminosities of the stars". Monthly Notices of the Royal Astronomical Society. 84 (5): 308–333. Bibcode:1924MNRAS..84..308E. doi:10.1093/mnras/84.5.308.

[24] [24]
Luyten, W.J. (1950). "The search for white dwarfs". The Astronomical Journal. 55: 86. Bibcode:1950AJ.....55...86L. doi:10.1086/106358.

[villanovar4-25] [25]
McCook, George P.; Sion, Edward M. (1999). "A catalog of spectroscopically identified white dwarfs". The Astrophysical Journal Supplement Series. 121 (1): 1–130. Bibcode:1999ApJS..121....1M. doi:10.1086/313186.

[sdssr4-26] [26]
Eisenstein, Daniel J.; Liebert, James; Harris, Hugh C.; Kleinman, S. J.; Nitta, Atsuko; Silvestri, Nicole; et al. (2006). "A catalog of spectroscopically confirmed white dwarfs from the Sloan Digital Sky Survey, data release 4". The Astrophysical Journal Supplement Series. 167 (1): 40–58. arXiv:astro-ph/0606700. Bibcode:2006ApJS..167...40E. doi:10.1086/507110. S2CID 13829139.

[27] [27]
Kilic, M.; Allende Prieto, C.; Brown, Warren R.; Koester, D. (2007). "The lowest mass white dwarf". The Astrophysical Journal. 660 (2): 1451–1461. arXiv:astro-ph/0611498. Bibcode:2007ApJ...660.1451K. doi:10.1086/514327. S2CID 18587748.

[sdsswd-28] [28]
Kepler, S.O.; Kleinman, S.J.; Nitta, A.; Koester, D.; Castanheira, B.G.; Giovannini, O.; Costa, A.F.M.; Althaus, L. (2007). "White dwarf mass distribution in the SDSS". Monthly Notices of the Royal Astronomical Society. 375 (4): 1315–1324. arXiv:astro-ph/0612277. Bibcode:2007MNRAS.375.1315K. doi:10.1111/j.1365-2966.2006.11388.x. S2CID 10892288.

[29] [29]
Shipman, H.L. (1979). "Masses and radii of white-dwarf stars. III – Results for 110 hydrogen-rich and 28 helium-rich stars". The Astrophysical Journal. 228: 240. Bibcode:1979ApJ...228..240S. doi:10.1086/156841.

[Saumon2022-30] [30]
Saumon, Didier; Blouin, Simon; Tremblay, Pier-Emmanuel (November 2022). "Current challenges in the physics of white dwarf stars". Physics Reports. 988: 1–63. arXiv:2209.02846. Bibcode:2022PhR...988....1S. doi:10.1016/j.physrep.2022.09.001. S2CID 252111027.

[31] [31]
Schmitt, Andreas (2010). Dense Matter in Compact Stars: A Pedagogical Introduction. Lecture Notes in Physics. Vol. 811. Springer. pp. 4, 143. arXiv:1001.3294. doi:10.1007/978-3-642-12866-0. ISBN 978-3-642-12866-0.

[32] [32]
Boss, L. (1910). Preliminary General Catalogue of 6188 stars for the epoch 1900. Carnegie Institution of Washington. Bibcode:1910pgcs.book.....B. LCCN 10009645 – via Archive.org.

[apj_630-33] [33]
Liebert, James; Young, P. A.; Arnett, D.; Holberg, J. B.; Williams, K. A. (2005). "The age and progenitor mass of Sirius B". The Astrophysical Journal. 630 (1): L69. arXiv:astro-ph/0507523. Bibcode:2005ApJ...630L..69L. doi:10.1086/462419. S2CID 8792889.

[34] [34]
Öpik, E. (1916). "The densities of visual binary stars". The Astrophysical Journal. 44: 292. Bibcode:1916ApJ....44..292O. doi:10.1086/142296.

[35] [35]
Eddington, A.S. (1927). Stars and Atoms. Clarendon Press. LCCN 27015694.

[36] [36]
Adams, W. S. (1925). "The Relativity Displacement of the Spectral Lines in the Companion of Sirius". Proceedings of the National Academy of Sciences. 11 (7): 382–387. Bibcode:1925PNAS...11..382A. doi:10.1073/pnas.11.7.382. PMC 1086032. PMID 16587023.

[CMS1999-37] [37]
Celotti, A.; Miller, J.C.; Sciama, D.W. (1999). "Astrophysical evidence for the existence of black holes". Class. Quantum Grav. 16 (12A): A3 – A21. arXiv:astro-ph/9912186. Bibcode:1999CQGra..16A...3C. doi:10.1088/0264-9381/16/12A/301. S2CID 17677758.

[38] [38]
Nave, C. R. "Nuclear Size and Density". HyperPhysics. Georgia State University. Archived from the original on 6 July 2009. Retrieved 26 June 2009.

[adams1997-39] [39]
Adams, Steve (1997). Relativity: an introduction to space-time physics. London; Bristol: CRC Press. p. 240. Bibcode:1997rist.book.....A. ISBN 978-0-7484-0621-0.

[fowler-40] [40]
Fowler, R. H. (1926). "On dense matter". Monthly Notices of the Royal Astronomical Society. 87 (2): 114–122. Bibcode:1926MNRAS..87..114F. doi:10.1093/mnras/87.2.114.

[41] [41]
Hoddeson, L. H.; Baym, G. (1980). "The Development of the Quantum Mechanical Electron Theory of Metals: 1900–28". Proceedings of the Royal Society of London. 371 (1744): 8–23. Bibcode:1980RSPSA.371....8H. doi:10.1098/rspa.1980.0051. JSTOR 2990270. S2CID 120476662.

[scibits-42] [42]
"Estimating Stellar Parameters from Energy Equipartition". ScienceBits. Archived from the original on 22 May 2012. Retrieved 9 May 2007.

[43] [43]
Bean, R. "Lecture 12 – Degeneracy pressure" (PDF). Lecture notes, Astronomy 211. Cornell University. Archived from the original (PDF) on 25 September 2007. Retrieved 21 September 2007.

[44] [44]
Anderson, W. (1929). "Über die Grenzdichte der Materie und der Energie". Zeitschrift für Physik (in German). 56 (11–12): 851–856. Bibcode:1929ZPhy...56..851A. doi:10.1007/BF01340146. S2CID 122576829.

[stoner-45] [45]
Stoner, C. (1930). "The Equilibrium of Dense Stars". Philosophical Magazine. 9: 944.

[chandra4-46] [46]
Chandrasekhar, S. (1931). "The Maximum Mass of Ideal White Dwarfs". The Astrophysical Journal. 74: 81. Bibcode:1931ApJ....74...81C. doi:10.1086/143324.

[chandra2-47] [47]
Chandrasekhar, S. (1935). "The highly collapsed configurations of a stellar mass (Second paper)". Monthly Notices of the Royal Astronomical Society. 95 (3): 207–225. Bibcode:1935MNRAS..95..207C. doi:10.1093/mnras/95.3.207.

[48] [48]
"The Nobel Prize in Physics 1983". The Nobel Foundation. Archived from the original on 6 May 2007. Retrieved 4 May 2007.

[49] [49]
Low, Andrew M. (2023). "The Chandrasekhar limit: a simplified approach". Physics Education. 58 (4): 045008. Bibcode:2023PhyEd..58d5008L. doi:10.1088/1361-6552/acdbb0.

[collapse-50] [50]
Canal, R.; Gutierrez, J. (1997). "The Possible White Dwarf-Neutron Star Connection". White Dwarfs. Astrophysics and Space Science Library. Vol. 214. pp. 49–55. arXiv:astro-ph/9701225. Bibcode:1997ASSL..214...49C. doi:10.1007/978-94-011-5542-7_7. ISBN 978-94-010-6334-0. S2CID 9288287.

[Chandrasekhar-51] [51]
Lieb, E. H.; Yau, H.-T. (1987). "A rigorous examination of the Chandrasekhar theory of stellar collapse". The Astrophysical Journal. 323 (1): 140–144. Bibcode:1987ApJ...323..140L. doi:10.1086/165813. Retrieved 20 March 2020.

[Mazzali2007-52] [52]
Mazzali, P. A.; Röpke, F. K.; Benetti, S.; Hillebrandt, W. (2007). "A Common Explosion Mechanism for Type Ia Supernovae". Science. 315 (5813): 825–828. arXiv:astro-ph/0702351. Bibcode:2007Sci...315..825M. doi:10.1126/science.1136259. PMID 17289993.

[53] [53]
Wheeler, J. C. (2000). Cosmic Catastrophes: Supernovae, Gamma-Ray Bursts, and Adventures in Hyperspace. Cambridge University Press. p. 96. ISBN 978-0-521-65195-0.

[Piro2014-54] [54]
Piro, A. L.; Thompson, T. A.; Kochanek, C. S. (2014). "Reconciling 56Ni production in Type Ia supernovae with double degenerate scenarios". Monthly Notices of the Royal Astronomical Society. 438 (4): 3456. arXiv:1308.0334. Bibcode:2014MNRAS.438.3456P. doi:10.1093/mnras/stt2451. S2CID 27316605.

[chen-55] [55]
Chen, W.-C.; Li, X.-D. (2009). "On the Progenitors of Super-Chandrasekhar Mass Type Ia Supernovae". The Astrophysical Journal. 702 (1): 686–691. arXiv:0907.0057. Bibcode:2009ApJ...702..686C. doi:10.1088/0004-637X/702/1/686. S2CID 14301164.

[56] [56]
Howell, D. A.; Sullivan, M.; Conley, A. J.; Carlberg, R. G. (2007). "Predicted and Observed Evolution in the Mean Properties of Type Ia Supernovae with Redshift". Astrophysical Journal Letters. 667 (1): L37 – L40. arXiv:astro-ph/0701912. Bibcode:2007ApJ...667L..37H. doi:10.1086/522030. S2CID 16667595.

[57] [57]
Coelho, Rodrigo C. V.; Calvão, Maurício O.; Reis, Ribamar R. R.; Siffert, Beatriz B. (2015). "Standardization of type Ia supernovae". European Journal of Physics. 36 (1): 015007. arXiv:1411.3596. Bibcode:2015EJPh...36a5007C. doi:10.1088/0143-0807/36/1/015007.

[58] [58]
Chabrier, G.; Baraffe, I. (2000). "Theory of low-Mass stars and substellar objects". Annual Review of Astronomy and Astrophysics. 38: 337–377. arXiv:astro-ph/0006383. Bibcode:2000ARA&A..38..337C. doi:10.1146/annurev.astro.38.1.337. S2CID 59325115.

[59] [59]
Kaler, J. "The Hertzsprung-Russell (HR) diagram". Archived from the original on 31 August 2009. Retrieved 5 May 2007.

[stds-60] [60]
"Basic symbols". Standards for Astronomical Catalogues, Version 2.0. VizieR. Archived from the original on 8 May 2017. Retrieved 12 January 2007.

[61] [61]
Tohline, J. E. "The Structure, Stability, and Dynamics of Self-Gravitating Systems". Archived from the original on 27 June 2010. Retrieved 30 May 2007.

[62] [62]
Hoyle, F. (1947). "Stars, Distribution and Motions of, Note on equilibrium configurations for rotating white dwarfs". Monthly Notices of the Royal Astronomical Society. 107 (2): 231–236. Bibcode:1947MNRAS.107..231H. doi:10.1093/mnras/107.2.231.

[63] [63]
Ostriker, J. P.; Bodenheimer, P. (1968). "Rapidly Rotating Stars. II. Massive White Dwarfs". The Astrophysical Journal. 151: 1089. Bibcode:1968ApJ...151.1089O. doi:10.1086/149507.

[64] [64]
Chanillo, Sagun; Li, Yan Yan (1994). "On diameters of uniformly rotating stars". Communications in Mathematical Physics. 166 (2): 417. Bibcode:1994CMaPh.166..417C. doi:10.1007/BF02112323. S2CID 8372549.

[65] [65]
Chanillo, Sagun; Weiss, Georg S. (2012). "A remark on the geometry of uniformly rotating stars". Journal of Differential Equations. 253 (2): 553. arXiv:1109.3046. Bibcode:2012JDE...253..553C. doi:10.1016/j.jde.2012.04.011. S2CID 144301.

[sionspectra-66] [66]
Sion, E. M.; Greenstein, J. L.; Landstreet, J. D.; Liebert, James; Shipman, H. L.; Wegner, G. A. (1983). "A proposed new white dwarf spectral classification system". The Astrophysical Journal. 269: 253. Bibcode:1983ApJ...269..253S. doi:10.1086/161036.

[cool-67] [67]
Hambly, N. C.; Smartt, S. J.; Hodgkin, S. T. (1997). "WD 0346+246: A Very Low Luminosity, Cool Degenerate in Taurus". The Astrophysical Journal. 489 (2): L157. Bibcode:1997ApJ...489L.157H. doi:10.1086/316797.

[wden-68] [68]
Fontaine, G.; Wesemael, F. (2001). "White dwarfs". In Murdin, P. (ed.). Encyclopedia of Astronomy and Astrophysics. IOP Publishing/Nature Publishing Group. ISBN 978-0-333-75088-9.

[69] [69]
Heise, J. (1985). "X-ray emission from isolated hot white dwarfs". Space Science Reviews. 40 (1–2): 79–90. Bibcode:1985SSRv...40...79H. doi:10.1007/BF00212870. S2CID 120431159.

[70] [70]
Lesaffre, P.; Podsiadlowski, Ph.; Tout, C. A. (2005). "A two-stream formalism for the convective Urca process". Monthly Notices of the Royal Astronomical Society. 356 (1): 131–144. arXiv:astro-ph/0411016. Bibcode:2005MNRAS.356..131L. doi:10.1111/j.1365-2966.2004.08428.x. S2CID 15797437.

[71] [71]
Mestel, L. (1952). "On the theory of white dwarf stars. I. The energy sources of white dwarfs". Monthly Notices of the Royal Astronomical Society. 112 (6): 583–597. Bibcode:1952MNRAS.112..583M. doi:10.1093/mnras/112.6.583.

[72] [72]
Kawaler, S. D. (1998). White Dwarf Stars and the Hubble Deep Field. The Hubble Deep Field: Proceedings of the Space Telescope Science Institute Symposium. p. 252. arXiv:astro-ph/9802217. Bibcode:1998hdf..symp..252K. ISBN 978-0-521-63097-9.

[73] [73]
Bergeron, P.; Ruiz, M. T.; Leggett, S. K. (1997). "The Chemical Evolution of Cool White Dwarfs and the Age of the Local Galactic Disk". The Astrophysical Journal Supplement Series. 108 (1): 339–387. Bibcode:1997ApJS..108..339B. doi:10.1086/312955.

[74] [74]
McCook, G. P.; Sion, E. M. (1999). "A Catalogue of Spectroscopically Identified White Dwarfs". The Astrophysical Journal Supplement Series. 121 (1): 1–130. Bibcode:1999ApJS..121....1M. doi:10.1086/313186.

[disklf-75] [75]
Leggett, S. K.; Ruiz, M. T.; Bergeron, P. (1998). "The Cool White Dwarf Luminosity Function and the Age of the Galactic Disk". The Astrophysical Journal. 497 (1): 294–302. Bibcode:1998ApJ...497..294L. doi:10.1086/305463.

[76] [76]
Gates, E.; Gyuk, G.; Harris, H. C.; Subbarao, M.; Anderson, S.; Kleinman, S. J.; et al. (2004). "Discovery of New Ultracool White Dwarfs in the Sloan Digital Sky Survey". The Astrophysical Journal. 612 (2): L129. arXiv:astro-ph/0405566. Bibcode:2004ApJ...612L.129G. doi:10.1086/424568. S2CID 7570539.

[Elms2022-77] [77]
Elms, Abbigail K.; Tremblay, Pier-Emmanuel; Gänsicke, Boris T.; Koester, Detlev; Hollands, Mark A.; Gentile Fusillo, Nicola Pietro; Cunningham, Tim; Apps, Kevin (1 December 2022). "Spectral analysis of ultra-cool white dwarfs polluted by planetary debris". Monthly Notices of the Royal Astronomical Society. 517 (3): 4557–4574. arXiv:2206.05258. Bibcode:2022MNRAS.517.4557E. doi:10.1093/mnras/stac2908. ISSN 0035-8711.

[78] [78]
Winget, D. E.; Hansen, C. J.; Liebert, James; Van Horn, H. M.; Fontaine, G.; Nather, R. E.; Kepler, S. O.; Lamb, D. Q. (1987). "An independent method for determining the age of the universe". The Astrophysical Journal. 315: L77. Bibcode:1987ApJ...315L..77W. doi:10.1086/184864. hdl:10183/108730.

[79] [79]
Trefil, J. S. (2004). The Moment of Creation: Big Bang Physics from Before the First Millisecond to the Present Universe. Dover Publications. ISBN 978-0-486-43813-9.

[Bergeron2022-80] [80]
Bergeron, P.; Kilic, Mukremin; Blouin, Simon; Bédard, A.; Leggett, S. K.; Brown, Warren R. (1 July 2022). "On the Nature of Ultracool White Dwarfs: Not so Cool after All". The Astrophysical Journal. 934 (1): 36. arXiv:2206.03174. Bibcode:2022ApJ...934...36B. doi:10.3847/1538-4357/ac76c7. ISSN 0004-637X.

[81] [81]
van Horn, H. M. (January 1968). "Crystallization of White Dwarfs". The Astrophysical Journal. 151: 227. Bibcode:1968ApJ...151..227V. doi:10.1086/149432.

[82] [82]
Barrat, J. L.; Hansen, J. P.; Mochkovitch, R. (1988). "Crystallization of carbon-oxygen mixtures in white dwarfs". Astronomy and Astrophysics. 199 (1–2): L15. Bibcode:1988A&A...199L..15B.

[83] [83]
Winget, D. E. (1995). "The Status of White Dwarf Asteroseismology and a Glimpse of the Road Ahead". Baltic Astronomy. 4 (2): 129. Bibcode:1995BaltA...4..129W. doi:10.1515/astro-1995-0209.

[84] [84]
Metcalfe, T. S.; Montgomery, M. H.; Kanaan, A. (20 April 2004). "Testing White Dwarf Crystallization Theory with Asteroseismology of the Massive Pulsating DA Star BPM 37093". The Astrophysical Journal. 605 (2): L133 – L136. arXiv:astro-ph/0402046. Bibcode:2004ApJ...605L.133M. doi:10.1086/420884. S2CID 119378552.

[lucy-85] [85]
Whitehouse, David (16 February 2004). "Diamond star thrills astronomers". BBC News. Archived from the original on 5 February 2007. Retrieved 6 January 2007.

[86] [86]
Kanaan, A.; Nitta, A.; Winget, D. E.; Kepler, S. O.; Montgomery, M. H.; Metcalfe, T. S.; et al. (2005). "Whole Earth Telescope observations of BPM 37093: A seismological test of crystallization theory in white dwarfs". Astronomy and Astrophysics. 432 (1): 219–224. arXiv:astro-ph/0411199. Bibcode:2005A&A...432..219K. doi:10.1051/0004-6361:20041125. S2CID 7297628.

[Brassard-87] [87]
Brassard, P.; Fontaine, G. (2005). "Asteroseismology of the Crystallized ZZ Ceti Star BPM 37093: A Different View". The Astrophysical Journal. 622 (1): 572–576. Bibcode:2005ApJ...622..572B. doi:10.1086/428116.

[88] [88]
Hansen, B. M. S.; Liebert, James (2003). "Cool White Dwarfs". Annual Review of Astronomy and Astrophysics. 41: 465. Bibcode:2003ARA&A..41..465H. doi:10.1146/annurev.astro.41.081401.155117.

[89] [89]
Antoine, Bédard; Simon, Blouin; Sihao, Cheng (2024). "Buoyant crystals halt the cooling of white dwarf stars". Nature. 627 (8003): 286–288. arXiv:2409.04419. Bibcode:2024Natur.627..286B. doi:10.1038/s41586-024-07102-y. ISSN 1476-4687. PMID 38448597.

[90] [90]
Althaus, L. G.; García-Berro, E.; Isern, J.; Córsico, A. H.; Miller Bertolami, M. M. (January 2012). "New phase diagrams for dense carbon-oxygen mixtures and white dwarf evolution". Astronomy & Astrophysics. 537: A33. arXiv:1110.5665. Bibcode:2012A&A...537A..33A. doi:10.1051/0004-6361/201117902. S2CID 119279832.

[91] [91]
Blouin, Simon; Daligault, Jérôme; Saumon, Didier (1 April 2021). "22 Ne Phase Separation as a Solution to the Ultramassive White Dwarf Cooling Anomaly". The Astrophysical Journal Letters. 911 (1): L5. arXiv:2103.12892. Bibcode:2021ApJ...911L...5B. doi:10.3847/2041-8213/abf14b. S2CID 232335433.

[92] [92]
Blouin, Simon; Daligault, Jérôme; Saumon, Didier; Bédard, Antoine; Brassard, Pierre (August 2020). "Toward precision cosmochronology: A new C/O phase diagram for white dwarfs". Astronomy & Astrophysics. 640: L11. arXiv:2007.13669. Bibcode:2020A&A...640L..11B. doi:10.1051/0004-6361/202038879. S2CID 220793255.

[93] [93]
Tremblay, P.-E.; Fontaine, G.; Fusillo, N. P. G.; Dunlap, B. H.; Gänsicke, B. T.; Hollands, M. H.; et al. (2019). "Core crystallization and pile-up in the cooling sequence of evolving white dwarfs" (PDF). Nature. 565 (7738): 202–205. arXiv:1908.00370. Bibcode:2019Natur.565..202T. doi:10.1038/s41586-018-0791-x. PMID 30626942. S2CID 58004893. Archived (PDF) from the original on 23 July 2019. Retrieved 23 July 2019.

[94] [94]
Chen, J.; et al. (2021). "Slowly cooling white dwarfs in M13 from stable hydrogen burning". Nature Astronomy. 5 (11): 1170–1177. arXiv:2109.02306. Bibcode:2021NatAs...5.1170C. doi:10.1038/s41550-021-01445-6.

[95] [95]
Istrate, A. G.; Tauris, T. M.; Langer, N.; Antoniadis, J. (2014). "The timescale of low-mass proto-helium white dwarf evolution". Astronomy and Astrophysics. 571: L3. arXiv:1410.5471. Bibcode:2014A&A...571L...3I. doi:10.1051/0004-6361/201424681. S2CID 55152203.

[96] [96]
"First Giant Planet around White Dwarf Found – ESO observations indicate the Neptune-like exoplanet is evaporating". www.eso.org. Archived from the original on 4 December 2019. Retrieved 4 December 2019.

[97] [97]
Schatzman, E. (1945). "Théorie du débit d'énergie des naines blanches". Annales d'Astrophysique. 8: 143. Bibcode:1945AnAp....8..143S.

[physrev-98] [98]
Koester, D.; Chanmugam, G. (1990). "Physics of white dwarf stars". Reports on Progress in Physics. 53 (7): 837–915. Bibcode:1990RPPh...53..837K. doi:10.1088/0034-4885/53/7/001. S2CID 122582479.

[kawaler-99] [99]
Kawaler, S. D. (1997). "White Dwarf Stars". In Kawaler, S. D.; Novikov, I.; Srinivasan, G. (eds.). Stellar remnants. 1997. ISBN 978-3-540-61520-0.

[100] [100]
Kuiper, G. P. (1941). "List of Known White Dwarfs". Publications of the Astronomical Society of the Pacific. 53 (314): 248. Bibcode:1941PASP...53..248K. doi:10.1086/125335.

[101] [101]
Luyten, W. J. (1952). "The Spectra and Luminosities of White Dwarfs". The Astrophysical Journal. 116: 283. Bibcode:1952ApJ...116..283L. doi:10.1086/145612.

[102] [102]
Greenstein, J. L. (1960). Stellar atmospheres. University of Chicago Press. Bibcode:1960stat.book.....G. LCCN 61-9138.

[103] [103]
Kepler, S. O.; Kleinman, S. J.; Nitta, A.; Koester, D.; Castanheira, B. G.; Giovannini, O.; Costa, A. F. M.; Althaus, L. (2007). "White dwarf mass distribution in the SDSS". Monthly Notices of the Royal Astronomical Society. 375 (4): 1315–1324. arXiv:astro-ph/0612277. Bibcode:2007MNRAS.375.1315K. doi:10.1111/j.1365-2966.2006.11388.x. S2CID 10892288.

[104] [104]
Dufour, P.; Liebert, James; Fontaine, G.; Behara, N. (2007). "White dwarf stars with carbon atmospheres". Nature. 450 (7169): 522–4. arXiv:0711.3227. Bibcode:2007Natur.450..522D. doi:10.1038/nature06318. PMID 18033290. S2CID 4398697.

[dwarf-105] [105]
Xu, S.; Jura, M.; Koester, D.; Klein, B.; Zuckerman, B. (2013). "Discovery of Molecular Hydrogen in White Dwarf Atmospheres". The Astrophysical Journal. 766 (2): L18. arXiv:1302.6619. Bibcode:2013ApJ...766L..18X. doi:10.1088/2041-8205/766/2/L18. S2CID 119248244.

[Weisskopf2007-106] [106]
Weisskopf, Martin C.; Wu, Kinwah; Trimble, Virginia; O’Dell, Stephen L.; Elsner, Ronald F.; Zavlin, Vyacheslav E.; Kouveliotou, Chryssa (10 March 2007). "A Chandra Search for Coronal X-Rays from the Cool White Dwarf GD 356". The Astrophysical Journal. 657 (2): 1026–1036. arXiv:astro-ph/0609585. Bibcode:2007ApJ...657.1026W. doi:10.1086/510776. ISSN 0004-637X.

[Route2024-107] [107]
Route, Matthew (20 December 2024). "The Decline and Fall of ROME. V. A Preliminary Search for Star-disrupted Planet Interactions and Coronal Activity at 5 GHz among White Dwarfs within 25 pc". The Astrophysical Journal. 977 (1): 261. arXiv:2411.13718. Bibcode:2024ApJ...977..261R. doi:10.3847/1538-4357/ad9567.

[:0-108] [108]
Jura, M.; Young, E.D. (1 January 2014). "Extrasolar Cosmochemistry". Annual Review of Earth and Planetary Sciences. 42 (1): 45–67. Bibcode:2014AREPS..42...45J. doi:10.1146/annurev-earth-060313-054740.

[109] [109]
Wilson, D.J.; Gänsicke, B.T.; Koester, D.; Toloza, O.; Pala, A. F.; Breedt, E.; Parsons, S.G. (11 August 2015). "The composition of a disrupted extrasolar planetesimal at SDSS J0845+2257 (Ton 345)". Monthly Notices of the Royal Astronomical Society. 451 (3): 3237–3248. arXiv:1505.07466. Bibcode:2015MNRAS.451.3237W. doi:10.1093/mnras/stv1201. S2CID 54049842.

[110] [110]
Blackett, P. M. S. (1947). "The Magnetic Field of Massive Rotating Bodies". Nature. 159 (4046): 658–66. Bibcode:1947Natur.159..658B. doi:10.1038/159658a0. PMID 20239729. S2CID 4133416.

[111] [111]
Lovell, B. (1975). "Patrick Maynard Stuart Blackett, Baron Blackett, of Chelsea. 18 November 1897 – 13 July 1974". Biographical Memoirs of Fellows of the Royal Society. 21: 1–115. doi:10.1098/rsbm.1975.0001. JSTOR 769678. S2CID 74674634.

[112] [112]
Landstreet, John D. (1967). "Synchrotron radiation of neutrinos and its astrophysical significance". Physical Review. 153 (5): 1372–1377. Bibcode:1967PhRv..153.1372L. doi:10.1103/PhysRev.153.1372.

[113] [113]
Ginzburg, V. L.; Zheleznyakov, V. V.; Zaitsev, V. V. (1969). "Coherent mechanisms of radio emission and magnetic models of pulsars". Astrophysics and Space Science. 4 (4): 464–504. Bibcode:1969Ap&SS...4..464G. doi:10.1007/BF00651351. S2CID 119003761.

[114] [114]
Kemp, J.C.; Swedlund, J.B.; Landstreet, J.D.; Angel, J.R.P. (1970). "Discovery of circularly polarized light from a white dwarf". The Astrophysical Journal. 161: L77. Bibcode:1970ApJ...161L..77K. doi:10.1086/180574.

[115] [115]
Ferrario, Lilia; de Martino, Domtilla; Gaensicke, Boris (2015). "Magnetic white dwarfs". Space Science Reviews. 191 (1–4): 111–169. arXiv:1504.08072. Bibcode:2015SSRv..191..111F. doi:10.1007/s11214-015-0152-0. S2CID 119057870.

[116] [116]
Kepler, S.O.; Pelisoli, I.; Jordan, S.; Kleinman, S.J.; Koester, D.; Kuelebi, B.; Pecanha, V.; Castanhiera, B.G.; Nitta, A.; Costa, J.E.S.; Winget, D.E.; Kanaan, A.; Fraga, L. (2013). "Magnetic white dwarf stars in the Sloan Digital Sky Survey". Monthly Notices of the Royal Astronomical Society. 429 (4): 2934–2944. arXiv:1211.5709. Bibcode:2013MNRAS.429.2934K. doi:10.1093/mnras/sts522. S2CID 53316287.

[117] [117]
Landstreet, J.D.; Bagnulo, S.; Valyavin, G.G.; Fossati, L.; Jordan, S.; Monin, D.; Wade, G.A. (2012). "On the incidence of weak magnetic fields in DA white dwarfs". Astronomy and Astrophysics. 545 (A30): 9pp. arXiv:1208.3650. Bibcode:2012A&A...545A..30L. doi:10.1051/0004-6361/201219829. S2CID 55153825.

[118] [118]
Liebert, James; Bergeron, P.; Holberg, J. B. (2003). "The True Incidence of Magnetism Among Field White Dwarfs". The Astronomical Journal. 125 (1): 348–353. arXiv:astro-ph/0210319. Bibcode:2003AJ....125..348L. doi:10.1086/345573. S2CID 9005227.

[119] [119]
Merali, Zeeya (19 July 2012). "Stars draw atoms closer together". Nature News & Comment. Nature. doi:10.1038/nature.2012.11045. Archived from the original on 20 July 2012. Retrieved 21 July 2012.

[120] [120]
Buckley, D.A.H.; Meintjes, P.J.; Potter, S.B.; Marsh, T.R.; Gänsicke, B.T. (23 January 2017). "Polarimetric evidence of a white dwarf pulsar in the binary system AR Scorpii". Nature Astronomy. 1 (2): 0029. arXiv:1612.03185. Bibcode:2017NatAs...1E..29B. doi:10.1038/s41550-016-0029. S2CID 15683792.

[121] [121]
Pelisoli, Ingrid; et al. (2023). "A 5.3-min-period pulsing white dwarf in a binary detected from radio to X-rays". Nature Astronomy. 7 (8): 931–942. arXiv:2306.09272. Bibcode:2023NatAs...7..931P. doi:10.1038/s41550-023-01995-x.

[122] [122]
"ZZ Ceti variables". Centre deDonnées astronomiques de Strasbourg. Association Française des Observateurs d'Etoiles Variables. Archived from the original on 5 February 2007. Retrieved 6 June 2007.

[quirion-123] [123]
Quirion, P.-O.; Fontaine, G.; Brassard, P. (2007). "Mapping the Instability Domains of GW Vir Stars in the Effective Temperature–Surface Gravity Diagram". The Astrophysical Journal Supplement Series. 171 (1): 219–248. Bibcode:2007ApJS..171..219Q. doi:10.1086/513870.

[124] [124]
Lawrence, G. M.; Ostriker, J. P.; Hesser, J. E. (1967). "Ultrashort-Period Stellar Oscillations. I. Results from White Dwarfs, Old Novae, Central Stars of Planetary Nebulae, 3c 273, and Scorpius XR-1". The Astrophysical Journal. 148: L161. Bibcode:1967ApJ...148L.161L. doi:10.1086/180037.

[125] [125]
Landolt, A. U. (1968). "A New Short-Period Blue Variable". The Astrophysical Journal. 153: 151. Bibcode:1968ApJ...153..151L. doi:10.1086/149645.

[126] [126]
Nagel, T.; Werner, K. (2004). "Detection of non-radial g-mode pulsations in the newly discovered PG 1159 star HE 1429-1209". Astronomy and Astrophysics. 426 (2): L45. arXiv:astro-ph/0409243. Bibcode:2004A&A...426L..45N. doi:10.1051/0004-6361:200400079. S2CID 9481357.

[127] [127]
O'Brien, M. S. (2000). "The Extent and Cause of the Pre–White Dwarf Instability Strip". The Astrophysical Journal. 532 (2): 1078–1088. arXiv:astro-ph/9910495. Bibcode:2000ApJ...532.1078O. doi:10.1086/308613. S2CID 115958740.

[128] [128]
Winget, D. E. (1998). "Asteroseismology of white dwarf stars". Journal of Physics: Condensed Matter. 10 (49): 11247–11261. Bibcode:1998JPCM...1011247W. doi:10.1088/0953-8984/10/49/014. S2CID 250749380.

[evo-129] [129]
Heger, A.; Fryer, C. L.; Woosley, S. E.; Langer, N.; Hartmann, D. H. (2003). "How Massive Single Stars End Their Life". The Astrophysical Journal. 591 (1): 288–300. arXiv:astro-ph/0212469. Bibcode:2003ApJ...591..288H. doi:10.1086/375341. S2CID 59065632.

[130] [130]
Napiwotzki, Ralf (2009). "The galactic population of white dwarfs". Journal of Physics. Conference Series. 172 (1): 012004. arXiv:0903.2159. Bibcode:2009JPhCS.172a2004N. doi:10.1088/1742-6596/172/1/012004. S2CID 17521113.

[Brown2011-131] [131]
Brown, J. M.; Kilic, M.; Brown, W. R.; Kenyon, S. J. (2011). "The binary fraction of low-mass white dwarfs". The Astrophysical Journal. 730 (67): 67. arXiv:1101.5169. Bibcode:2011ApJ...730...67B. doi:10.1088/0004-637X/730/2/67.

[132] [132]
Laughlin, G.; Bodenheimer, P.; Adams, Fred C. (1997). "The End of the Main Sequence". The Astrophysical Journal. 482 (1): 420–432. Bibcode:1997ApJ...482..420L. doi:10.1086/304125.

[sj-133] [133]
Jeffery, Simon. "Stars Beyond Maturity". Archived from the original on 4 April 2015. Retrieved 3 May 2007.

[134] [134]
Sarna, M. J.; Ergma, E.; Gerškevitš, J. (2001). "Helium core white dwarf evolution – including white dwarf companions to neutron stars". Astronomische Nachrichten. 322 (5–6): 405–410. Bibcode:2001AN....322..405S. doi:10.1002/1521-3994(200112)322:5/6<405::AID-ASNA405>3.0.CO;2-6.

[135] [135]
Benvenuto, O. G.; De Vito, M. A. (2005). "The formation of helium white dwarfs in close binary systems – II". Monthly Notices of the Royal Astronomical Society. 362 (3): 891–905. Bibcode:2005MNRAS.362..891B. doi:10.1111/j.1365-2966.2005.09315.x.

[136] [136]
Nelemans, G.; Tauris, T. M. (1998). "Formation of undermassive single white dwarfs and the influence of planets on late stellar evolution". Astronomy and Astrophysics. 335: L85. arXiv:astro-ph/9806011. Bibcode:1998A&A...335L..85N.

[137] [137]
Zhang, Xianfei; Hall, Philip D.; Jeffery, C. Simon; Bi, Shaolan (2018). "Evolution models of helium white dwarf–main-sequence star merger remnants: the mass distribution of single low-mass white dwarfs". Monthly Notices of the Royal Astronomical Society. 474: 427–432. arXiv:1711.03285. doi:10.1093/mnras/stx2747.

[Woolsey2002-138] [138]
Woosley, S. E.; Heger, A.; Weaver, T. A. (2002). "The evolution and explosion of massive stars". Reviews of Modern Physics. 74 (4): 1015–1071. Bibcode:2002RvMP...74.1015W. doi:10.1103/RevModPhys.74.1015.

[vd1-139] [139]
Dhillon, Vik. "The evolution of low-mass stars". lecture notes, Physics 213. University of Sheffield. Archived from the original on 7 November 2012. Retrieved 3 May 2007.

[vd2-140] [140]
Dhillon, Vik. "The evolution of high-mass stars". lecture notes, Physics 213. University of Sheffield. Archived from the original on 7 November 2012. Retrieved 3 May 2007.

[141] [141]
Schaffner-Bielich, Jürgen (2005). "Strange quark matter in stars: A general overview". Journal of Physics G: Nuclear and Particle Physics. 31 (6): S651 – S657. arXiv:astro-ph/0412215. Bibcode:2005JPhG...31S.651S. doi:10.1088/0954-3899/31/6/004. S2CID 118886040.

[142] [142]
Nomoto, K. (1984). "Evolution of 8–10 solar mass stars toward electron capture supernovae. I – Formation of electron-degenerate O + NE + MG cores". The Astrophysical Journal. 277: 791. Bibcode:1984ApJ...277..791N. doi:10.1086/161749.

[143] [143]
Werner, K.; Rauch, T.; Barstow, M. A.; Kruk, J. W. (2004). "Chandra and FUSE spectroscopy of the hot bare stellar core H?1504+65". Astronomy and Astrophysics. 421 (3): 1169–1183. arXiv:astro-ph/0404325. Bibcode:2004A&A...421.1169W. doi:10.1051/0004-6361:20047154. S2CID 2983893.

[144] [144]
Livio, Mario; Truran, James W. (1994). "On the interpretation and implications of nova abundances: An abundance of riches or an overabundance of enrichments". The Astrophysical Journal. 425: 797. Bibcode:1994ApJ...425..797L. doi:10.1086/174024.

[ironcore-145] [145]
Jordan, George C. IV.; Perets, Hagai B.; Fisher, Robert T.; van Rossum, Daniel R. (2012). "Failed-detonation Supernovae: Subluminous Low-velocity Ia Supernovae and their Kicked Remnant White Dwarfs with Iron-rich Cores". The Astrophysical Journal Letters. 761 (2): L23. arXiv:1208.5069. Bibcode:2012ApJ...761L..23J. doi:10.1088/2041-8205/761/2/L23. S2CID 119203015.

[ironcore2-146] [146]
Panei, J. A.; Althaus, L. G.; Benvenuto, O. G. (2000). "The evolution of iron-core white dwarfs". Monthly Notices of the Royal Astronomical Society. 312 (3): 531–539. arXiv:astro-ph/9911371. Bibcode:2000MNRAS.312..531P. doi:10.1046/j.1365-8711.2000.03236.x. S2CID 17854858.

[fate-147] [147]
Adams, Fred C.; Laughlin, Gregory (1997). "A dying universe: The long-term fate and evolution of astrophysical objects". Reviews of Modern Physics. 69 (2): 337–372. arXiv:astro-ph/9701131. Bibcode:1997RvMP...69..337A. doi:10.1103/RevModPhys.69.337. S2CID 12173790.

[2007ApJ...669.1279S-148] [148]
Seager, S.; Kuchner, M.; Hier-Majumder, C.; Militzer, B. (19 July 2007). "Mass-Radius Relationships for Solid Exoplanets". The Astrophysical Journal. 669 (2) (published November 2007): 1279–1297. arXiv:0707.2895. Bibcode:2007ApJ...669.1279S. doi:10.1086/521346. S2CID 8369390.

[149] [149]
Bailes, M.; et al. (2011). "Transformation of a Star into a Planet in a Millisecond Pulsar Binary". Science. 333 (6050): 1717–1720. arXiv:1108.5201. Bibcode:2011Sci...333.1717B. doi:10.1126/science.1208890. PMID 21868629.

[TIME-2011-08-26-150] [150]
Lemonick, Michael (26 August 2011). "Scientists Discover a Diamond as Big as a Planet". Time Magazine. Archived from the original on 24 August 2013. Retrieved 18 June 2015.

[151] [151]
"Hubble finds dead stars "polluted" with planetary debris". ESA/Hubble Press Release. Archived from the original on 9 June 2013. Retrieved 10 May 2013.

[152] [152]
"Comet falling into white dwarf (artist's impression)". www.spacetelescope.org. Archived from the original on 15 February 2017. Retrieved 14 February 2017.

[153] [153]
Koester, D.; Gänsicke, B. T.; Farihi, J. (1 June 2014). "The frequency of planetary debris around young white dwarfs". Astronomy and Astrophysics. 566: A34. arXiv:1404.2617. Bibcode:2014A&A...566A..34K. doi:10.1051/0004-6361/201423691. ISSN 0004-6361. S2CID 119268896.

[154] [154]
Jura, M. (1 May 2008). "Pollution of Single White Dwarfs by Accretion of Many Small Asteroids". The Astronomical Journal. 135 (5): 1785–1792. arXiv:0802.4075. Bibcode:2008AJ....135.1785J. doi:10.1088/0004-6256/135/5/1785. ISSN 0004-6256. S2CID 16571761.

[:2-155] [155]
Debes, John H.; Thévenot, Melina; Kuchner, Marc J.; Burgasser, Adam J.; Schneider, Adam C.; Meisner, Aaron M.; Gagné, Jonathan; Faherty, Jacqueline K.; Rees, Jon M. (19 February 2019). "A 3 Gyr White Dwarf with Warm Dust Discovered via the Backyard Worlds: Planet 9 Citizen Science Project". The Astrophysical Journal. 872 (2): L25. arXiv:1902.07073. Bibcode:2019ApJ...872L..25D. doi:10.3847/2041-8213/ab0426. ISSN 2041-8213. S2CID 119359995.

[156] [156]
van Maanen, A. (1 December 1917). "Two Faint Stars with Large Proper Motion". Publications of the Astronomical Society of the Pacific. 29 (172): 258. Bibcode:1917PASP...29..258V. doi:10.1086/122654. ISSN 0004-6280. S2CID 250734202.

[Klein_61-157] [157]
Klein, Beth L.; Doyle, Alexandra E.; Zuckerman, B.; Dufour, P.; Blouin, Simon; Melis, Carl; Weinberger, Alycia J.; Young, Edward D. (1 June 2021). "Discovery of Beryllium in White Dwarfs Polluted by Planetesimal Accretion". The Astrophysical Journal. 914 (1): 61. arXiv:2102.01834. Bibcode:2021ApJ...914...61K. doi:10.3847/1538-4357/abe40b. ISSN 0004-637X. S2CID 231786441.

[158] [158]
Zuckerman, B. (1 June 2015). Recognition of the First Observational Evidence of an Extrasolar Planetary System. 19Th European Workshop on White Dwarfs. Vol. 493. p. 291. Bibcode:2015ASPC..493..291Z.

[159] [159]
Farihi, J. (1 April 2016). "Circumstellar debris and pollution at white dwarf stars". New Astronomy Reviews. 71: 9–34. arXiv:1604.03092. Bibcode:2016NewAR..71....9F. doi:10.1016/j.newar.2016.03.001. ISSN 1387-6473. S2CID 118486264.

[160] [160]
Zuckerman, B.; Becklin, E. E. (1 November 1987). "Excess infrared radiation from a white dwarf—an orbiting brown dwarf?". Nature. 330 (6144): 138–140. Bibcode:1987Natur.330..138Z. doi:10.1038/330138a0. ISSN 0028-0836. S2CID 4357883.

[:3-161] [161]
Reach, William T.; Kuchner, Marc J.; Von Hippel, Ted; Burrows, Adam; Mullally, Fergal; Kilic, Mukremin; Winget, D. E. (2005). "The Dust Cloud around the White Dwarf G29-38". The Astrophysical Journal. 635 (2): L161. arXiv:astro-ph/0511358. Bibcode:2005ApJ...635L.161R. doi:10.1086/499561. S2CID 119462589.

[162] [162]
Steckloff, Jordan K.; Debes, John; Steele, Amy; Johnson, Brandon; Adams, Elisabeth R.; Jacobson, Seth A.; Springmann, Alessondra (1 June 2021). "How Sublimation Delays the Onset of Dusty Debris Disk Formation around White Dwarf Stars". The Astrophysical Journal. 913 (2): L31. arXiv:2104.14035. Bibcode:2021ApJ...913L..31S. doi:10.3847/2041-8213/abfd39. ISSN 0004-637X. PMC 8740607. PMID 35003618.

[:4-163] [163]
Veras, Dimitri (1 October 2021). "Planetary Systems Around White Dwarfs". Oxford Research Encyclopedia of Planetary Science. Oxford University Press. arXiv:2106.06550. Bibcode:2021orel.bookE...1V. doi:10.1093/acrefore/9780190647926.013.238. ISBN 978-0-19-064792-6.

[Mullally2024-164] [164]
Mullally, Susan E.; Debes, John; Cracraft, Misty; Mullally, Fergal; Poulsen, Sabrina; Albert, Loic; Thibault, Katherine; Reach, William T.; Hermes, J. J.; Barclay, Thomas; Kilic, Mukremin; Quintana, Elisa V. (24 January 2024). "JWST Directly Images Giant Planet Candidates Around Two Metal-Polluted White Dwarf Stars". The Astrophysical Journal Letters. 962 (2): L32. arXiv:2401.13153. Bibcode:2024ApJ...962L..32M. doi:10.3847/2041-8213/ad2348.

[165] [165]
"Comet clash kicks up dusty haze". BBC News. 13 February 2007. Archived from the original on 16 February 2007. Retrieved 20 September 2007.

[166] [166]
Su, K. Y. L.; Chu, Y.-H.; Rieke, G. H.; Huggins, P. J.; Gruendl, R.; Napiwotzki, R.; Rauch, T.; Latter, W. B.; Volk, K. (2007). "A Debris Disk around the Central Star of the Helix Nebula?". The Astrophysical Journal. 657 (1): L41. arXiv:astro-ph/0702296. Bibcode:2007ApJ...657L..41S. doi:10.1086/513018. S2CID 15244406.

[167] [167]
Sion, Edward M.; Holberg, J.B.; Oswalt, Terry D.; McCook, George P.; Wasatonic, Richard (2009). "The White Dwarfs Within 20 Parsecs of the Sun: Kinematics and Statistics". The Astronomical Journal. 138 (6): 1681–1689. arXiv:0910.1288. Bibcode:2009AJ....138.1681S. doi:10.1088/0004-6256/138/6/1681. S2CID 119284418.

[168] [168]
Li, Jianke; Ferrario, Lilia; Wickramasinghe, Dayal (1998). "Planets around White Dwarfs". Astrophysical Journal Letters. 503 (1): L151. Bibcode:1998ApJ...503L.151L. doi:10.1086/311546. p. L51.

[169] [169]
Debes, John H.; Walsh, Kevin J.; Stark, Christopher (24 February 2012). "The Link Between Planetary Systems, Dusty White Dwarfs, and Metal-Polluted White Dwarfs". The Astrophysical Journal. 747 (2): 148. arXiv:1201.0756. Bibcode:2012ApJ...747..148D. doi:10.1088/0004-637X/747/2/148. ISSN 0004-637X. S2CID 118688656.

[170] [170]
Veras, Dimitri; Gänsicke, Boris T. (21 February 2015). "Detectable close-in planets around white dwarfs through late unpacking". Monthly Notices of the Royal Astronomical Society. 447 (2): 1049–1058. arXiv:1411.6012. Bibcode:2015MNRAS.447.1049V. doi:10.1093/mnras/stu2475. ISSN 0035-8711. S2CID 119279872.

[171] [171]
Frewen, S. F. N.; Hansen, B. M. S. (11 April 2014). "Eccentric planets and stellar evolution as a cause of polluted white dwarfs". Monthly Notices of the Royal Astronomical Society. 439 (3): 2442–2458. arXiv:1401.5470. Bibcode:2014MNRAS.439.2442F. doi:10.1093/mnras/stu097. ISSN 0035-8711. S2CID 119257046.

[172] [172]
Bonsor, Amy; Gänsicke, Boris T.; Veras, Dimitri; Villaver, Eva; Mustill, Alexander J. (21 May 2018). "Unstable low-mass planetary systems as drivers of white dwarf pollution". Monthly Notices of the Royal Astronomical Society. 476 (3): 3939–3955. arXiv:1711.02940. Bibcode:2018MNRAS.476.3939M. doi:10.1093/mnras/sty446. ISSN 0035-8711. S2CID 4809366.

[173] [173]
Gänsicke, Boris T.; Holman, Matthew J.; Veras, Dimitri; Payne, Matthew J. (21 March 2016). "Liberating exomoons in white dwarf planetary systems". Monthly Notices of the Royal Astronomical Society. 457 (1): 217–231. arXiv:1603.09344. Bibcode:2016MNRAS.457..217P. doi:10.1093/mnras/stv2966. ISSN 0035-8711. S2CID 56091285.

[174] [174]
Rebassa-Mansergas, Alberto; Xu (许偲艺), Siyi; Veras, Dimitri (21 January 2018). "The critical binary star separation for a planetary system origin of white dwarf pollution". Monthly Notices of the Royal Astronomical Society. 473 (3): 2871–2880. arXiv:1708.05391. Bibcode:2018MNRAS.473.2871V. doi:10.1093/mnras/stx2141. ISSN 0035-8711. S2CID 55764122.

[175] [175]
Becklin, E. E.; Zuckerman, B.; Farihi, J. (10 February 2008). "Spitzer IRAC Observations of White Dwarfs. I. Warm Dust at Metal-Rich Degenerates". The Astrophysical Journal. 674 (1): 431–446. arXiv:0710.0907. Bibcode:2008ApJ...674..431F. doi:10.1086/521715. ISSN 0004-637X. S2CID 17813180.

[176] [176]
Lemonick, Michael D. (21 October 2015). "Zombie Star Caught Feasting on Asteroids". National Geographic News. Archived from the original on 24 October 2015. Retrieved 22 October 2015.

[:1-177] [177]
Vanderburg, Andrew; Johnson, John Asher; Rappaport, Saul; Bieryla, Allyson; Irwin, Jonathan; Lewis, John Arban; Kipping, David; Brown, Warren R.; Dufour, Patrick (22 October 2015). "A disintegrating minor planet transiting a white dwarf". Nature. 526 (7574): 546–549. arXiv:1510.06387. Bibcode:2015Natur.526..546V. doi:10.1038/nature15527. PMID 26490620. S2CID 4451207.

[Gänsicke-178] [178]
Gänsicke, Boris T.; Schreiber, Matthias R.; Toloza, Odette; Gentile Fusillo, Nicola P.; Koester, Detlev; Manser, Christopher J. "Accretion of a giant planet onto a white dwarf" (PDF). ESO. Archived (PDF) from the original on 4 December 2019. Retrieved 11 December 2019.

[:5-179] [179]
Wang, Ting-Gui; Jiang, Ning; Ge, Jian; Cutri, Roc M.; Jiang, Peng; Sheng, Zhengfeng; Zhou, Hongyan; Bauer, James; Mainzer, Amy; Wright, Edward L. (November 2019). "An On-going Mid-infrared Outburst in the White Dwarf 0145+234: Catching in Action of Tidal Disruption of an Exoasteroid?". Astrophysical Journal Letters. 886 (1): L5. arXiv:1910.04314. Bibcode:2019ApJ...886L...5W. doi:10.3847/2041-8213/ab53ed.

[Vanderburg2020-180] [180]
Vanderburg, Andrew; Rappaport, Saul A.; Xu, Siyi; Crossfield, Ian J. M.; Becker, Juliette C.; Gary, Bruce; et al. (September 2020). "A giant planet candidate transiting a white dwarf". Nature. 585 (7825): 363–367. arXiv:2009.07282. Bibcode:2020Natur.585..363V. doi:10.1038/s41586-020-2713-y. PMID 32939071.

[181] [181]
Kipping, David (January 2024). "The giant nature of WD 1856 b implies that transiting rocky planets are rare around white dwarfs". Monthly Notices of the Royal Astronomical Society. 527 (2): 3532–3541. arXiv:2310.15219. doi:10.1093/mnras/stad3431.

[Blackman2021-182] [182]
Blackman, J. W.; Beaulieu, J. P.; Bennett, D. P.; Danielski, C.; Alard, C.; Cole, A. A.; Vandorou, A.; Ranc, C.; Terry, S. K.; Bhattacharya, A.; Bond, I.; Bachelet, E.; Veras, D.; Koshimoto, N.; Batista, V.; Marquette, J. B. (2021). "A Jovian analogue orbiting a white dwarf star". Nature. 598 (7880): 272–275. arXiv:2110.07934. Bibcode:2021Natur.598..272B. doi:10.1038/s41586-021-03869-6. PMID 34646001.

[183] [183]
Kervella, Pierre; Arenou, Frédéric; Mignard, François; Thévenin, Frédéric (1 March 2019). "Stellar and substellar companions of nearby stars from Gaia DR2. Binarity from proper motion anomaly". Astronomy and Astrophysics. 623: A72. arXiv:1811.08902. Bibcode:2019A&A...623A..72K. doi:10.1051/0004-6361/201834371. ISSN 0004-6361. S2CID 119491061.

[184] [184]
Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (1 January 2022). "Stellar and substellar companions from Gaia EDR3. Proper-motion anomaly and resolved common proper-motion pairs". Astronomy and Astrophysics. 657: A7. arXiv:2109.10912. Bibcode:2022A&A...657A...7K. doi:10.1051/0004-6361/202142146. ISSN 0004-6361. S2CID 237605138.

[GaiaDR3-185] [185]
Gaia Collaboration; Arenou, F.; Babusiaux, C.; Barstow, M. A.; Faigler, S.; Jorissen, A.; Kervella, P.; Mazeh, T.; Mowlavi, N.; Panuzzo, P.; Sahlmann, J.; Shahaf, S.; Sozzetti, A.; Bauchet, N.; Damerdji, Y. (2023). "Gaia Data Release 3". Astronomy & Astrophysics. 674: A34. arXiv:2206.05595. doi:10.1051/0004-6361/202243782. S2CID 249626026.

[186] [186]
"CYCLE 2 GO". STScI.edu. Retrieved 15 May 2023.

[187] [187]
"Gaia DR3 known issues". ESA. 5 May 2023. Retrieved 8 August 2023. During validation of epoch astrometry for Gaia DR4, an error was discovered, that had already had an impact on the Gaia DR3 non-single star results. [...] We can conclude that the solutions for [...] WD 0141-675 [...] are false-positives as far as Gaia non-single star processing is concerned.

[188] [188]
Casewell, S. L.; Debes, J.; Dupuy, T. J.; Dufour, P.; Bonsor, A.; Rebassa-Mansergas, A.; Murillo-Ojeda, R.; French, J. R.; Xu, Siyi (许偲艺); Martin, E.; Manjavacas, E. (8 April 2024). "PHL 5038AB: Is the brown dwarf causing pollution of its white dwarf host star?". MNRAS. 530 (3): 3302–3309. arXiv:2404.05488. doi:10.1093/mnras/stae974.

[189] [189]
Agol, Eric (2011). "Transit Surveys for Earths in the Habitable Zones of White Dwarfs". The Astrophysical Journal Letters. 635 (2): L31. arXiv:1103.2791. Bibcode:2011ApJ...731L..31A. doi:10.1088/2041-8205/731/2/L31. S2CID 118739494.

[190] [190]
Barnes, Rory; Heller, René (2011). "Habitable Planets Around White and Brown Dwarfs: The Perils of a Cooling Primary". Astrobiology. 13 (3): 279–291. arXiv:1211.6467. Bibcode:2013AsBio..13..279B. doi:10.1089/ast.2012.0867. PMC 3612282. PMID 23537137.

[191] [191]
Nordhaus, J.; Spiegel, D.S. (2013). "On the orbits of low-mass companions to white dwarfs and the fates of the known exoplanets". Monthly Notices of the Royal Astronomical Society. 432 (1): 500–505. arXiv:1211.1013. Bibcode:2013MNRAS.432..500N. doi:10.1093/mnras/stt569. S2CID 119227364.

[di_stefano_et_al1997-192] [192]
Di Stefano, R.; Nelson, L. A.; Lee, W.; Wood, T. H.; Rappaport, S. (1997). "Luminous Supersoft X-ray Sources as Type Ia Progenitors". In P. Ruiz-Lapuente; R. Canal; J. Isern (eds.). Thermonuclear Supernovae. NATO Science Series C: Mathematical and physical sciences. Vol. 486. Springer. pp. 148–149. Bibcode:1997ASIC..486..147D. doi:10.1007/978-94-011-5710-0_10. ISBN 978-0-7923-4359-2.

[193] [193]
Lopes de Oliveira, R.; Bruch, A.; Rodrigues, C. V.; de Oliveira, A. S.; Mukai, K. (2020). "CTCV J2056-3014: An X-Ray-faint Intermediate Polar Harboring an Extremely Fast-spinning White Dwarf". The Astrophysical Journal Letters. 898 (2): L40. arXiv:2007.13932. Bibcode:2020ApJ...898L..40L. doi:10.3847/2041-8213/aba618. S2CID 220831174.

[hscfa20101116-194] [194]
Aguilar, David A.; Pulliam, Christine (16 November 2010). "Astronomers Discover Merging Star Systems that Might Explode". Harvard-Smithsonian Center for Astrophysics. Archived from the original on 9 April 2011. Retrieved 16 February 2011.

[hscfa20110713-195] [195]
Aguilar, David A.; Pulliam, Christine (13 July 2011). "Evolved Stars Locked in Fatalistic Dance". Harvard-Smithsonian Center for Astrophysics. Archived from the original on 15 July 2011. Retrieved 17 July 2011.

[196] [196]
Yoon, S.-C.; Langer, N. (2004). "Presupernova evolution of accreting white dwarfs with rotation". Astronomy and Astrophysics. 419 (2): 623–644. arXiv:astro-ph/0402287. Bibcode:2004A&A...419..623Y. doi:10.1051/0004-6361:20035822. S2CID 2963085.

[sniamodels-197] [197]
Hillebrandt, W.; Niemeyer, J. C. (2000). "Type IA supernova explosion models". Annual Review of Astronomy and Astrophysics. 38: 191–230. arXiv:astro-ph/0006305. Bibcode:2000ARA&A..38..191H. doi:10.1146/annurev.astro.38.1.191.

[198] [198]
Blinnikov, S. I.; Röpke, F. K.; Sorokina, E. I.; Gieseler, M.; Reinecke, M.; Travaglio, C.; Hillebrandt, W.; Stritzinger, M. (2006). "Theoretical light curves for deflagration models of type Ia supernova". Astronomy and Astrophysics. 453 (1): 229–240. arXiv:astro-ph/0603036. Bibcode:2006A&A...453..229B. doi:10.1051/0004-6361:20054594. S2CID 15493284.

[:6-199] [199]
Maoz, D.; Mannucci, F. (18 January 2012). "Type-Ia Supernova Rates and the Progenitor Problem: A Review". Publications of the Astronomical Society of Australia. 29 (4): 447–465. arXiv:1111.4492. Bibcode:2012PASA...29..447M. doi:10.1071/AS11052. ISSN 1448-6083.

[:7-200] [200]
Wang, Bo; Han, Zhanwen (1 June 2012). "Progenitors of type Ia supernovae". New Astronomy Reviews. 56 (4): 122–141. arXiv:1204.1155. Bibcode:2012NewAR..56..122W. doi:10.1016/j.newar.2012.04.001. ISSN 1387-6473.

[201] [201]
Maoz, Dan; Mannucci, Filippo; Nelemans, Gijs (18 August 2014). "Observational Clues to the Progenitors of Type Ia Supernovae". Annual Review of Astronomy and Astrophysics. 52 (1): 107–170. arXiv:1312.0628. Bibcode:2014ARA&A..52..107M. doi:10.1146/annurev-astro-082812-141031. ISSN 0066-4146.

[hernandez2012-202] [202]
González Hernández, J.I.; Ruiz-Lapuente, P.; Tabernero, H. M.; Montes, D.; Canal, R.; Méndez, J.; Bedin, L. R. (2012). "No surviving evolved companions of the progenitor of SN 1006". Nature. 489 (7417): 533–536. arXiv:1210.1948. Bibcode:2012Natur.489..533G. doi:10.1038/nature11447. PMID 23018963. S2CID 4431391.

[Krause2008-203] [203]
Krause, Oliver; et al. (2008). "Tycho Brahe's 1572 supernova as a standard type Ia as revealed by its light-echo spectrum". Nature. 456 (7222): 617–619. arXiv:0810.5106. Bibcode:2008Natur.456..617K. doi:10.1038/nature07608. PMID 19052622. S2CID 4409995.

[dlFM2022-204] [204]
de la Fuente Marcos, Raúl; de la Fuente Marcos, Carlos (2022). "Deep and fast Solar System flybys: The controversial case of WD 0810-353". Astronomy & Astrophysics. 668: A14. arXiv:2210.04863. Bibcode:2022A&A...668A..14D. doi:10.1051/0004-6361/202245020. ISSN 0004-6361. S2CID 252863734.

[205] [205]
Landstreet, J. D.; Villaver, E.; Bagnulo, S. (2023). "Not so fast, not so furious: just magnetic". The Astrophysical Journal. 952 (2): 129. arXiv:2306.11663. Bibcode:2023ApJ...952..129L. doi:10.3847/1538-4357/acdac8.

[206] [206]
Kruckow, Matthias U.; Neunteufel, Patrick G.; Di Stefano, Rosanne; Gao, Yan; Kobayashi, Chiaki (2021). "A Catalog of Potential Post–Common Envelope Binaries". The Astrophysical Journal. 920 (2): 86. arXiv:2107.05221. Bibcode:2021ApJ...920...86K. doi:10.3847/1538-4357/ac13ac.

[207] [207]
Nordhaus, J.; Wellons, S.; Spiegel, D. S.; Metzger, B. D.; Blackman, E. G. (2011). "Formation of high-field magnetic white dwarfs from common envelopes". PNAS. 108 (8): 3135–3140. arXiv:1010.1529. Bibcode:2011PNAS..108.3135N. doi:10.1073/pnas.1015005108. PMC 3044383. PMID 21300910.

[208] [208]
Rebassa-Mansergas, A.; Solano, E.; Jiménez-Esteban, F. M.; Torres, S.; Rodrigo, C.; Ferrer-Burjachs, A.; Calcaferro, L. M.; Althaus, L. G.; Córsico, A. H. (October 2021). "White dwarf–main-sequence binaries from Gaia EDR3: the unresolved 100 pc volume-limited sample". Monthly Notices of the Royal Astronomical Society. 506 (4): 5201–5211. arXiv:2107.06303. doi:10.1093/mnras/stab2039.

[209] [209]
Schreiber, M. R.; Gänsicke, B. T. (2003). "The age, life expectancy, and space density of Post Common Envelope Binaries". Astronomy and Astrophysics. 406: 305–321. arXiv:astro-ph/0305531. Bibcode:2003A&A...406..305S. doi:10.1051/0004-6361:20030801.

[nasa1-210] [210]
"Cataclysmic Variables". fact sheet. Imagine the Universe!. NASA Goddard. Archived from the original on 9 July 2007. Retrieved 4 May 2007.

[nasa2-211] [211]
"Introduction to Cataclysmic Variables (CVs)". fact sheet. NASA Goddard. Archived from the original on 6 February 2012. Retrieved 4 May 2007.

[212] [212]
Fraknoi, Andrew; et al. (2024). "18.4 The H–R Diagram". Astronomy 2e. OpenStax. p. 618. ISBN 978-1-951693-50-3.

[213] [213]
Perpinyà-Vallès, M.; Rebassa-Mansergas, A.; Gänsicke, B. T.; Toonen, S.; Hermes, J. J.; Gentile Fusillo, N. P.; Tremblay, P.-E. (February 2019). "Discovery of the first resolved triple white dwarf". Monthly Notices of the Royal Astronomical Society. 483 (1): 901–907. arXiv:1811.07752. doi:10.1093/mnras/sty3149.

[214] [214]
Brandner, Wolfgang; Zinnecker, Hans; Kopytova, Taisiya (2021). "Search for giant planets around seven white dwarfs in the Hyades cluster with the Hubble Space Telescope". Monthly Notices of the Royal Astronomical Society. 500 (3): 3920–3925. arXiv:2011.03562. doi:10.1093/mnras/staa3422.

[215] [215]
Luhman, K. L.; Burgasser, A. J.; Bochanski, J. J. (2011). "Discovery of a Candidate for the Coolest Known Brown Dwarf". The Astrophysical Journal Letters. 730 (1): L9. arXiv:1102.5411. Bibcode:2011ApJ...730L...9L. doi:10.1088/2041-8205/730/1/L9.

[216] [216]
Rodriguez, David R.; Zuckerman, B.; Melis, Carl; Song, Inseok (May 2011). "The Ultra Cool Brown Dwarf Companion of WD 0806-661B: Age, Mass, and Formation Mechanism". The Astrophysical Journal Letters. 732 (2): L29. arXiv:1103.3544. Bibcode:2011ApJ...732L..29R. doi:10.1088/2041-8205/732/2/L29.

[217] [217]
Veras, Dimitri; Evans, N. Wyn (21 March 2013). "Exoplanets beyond the Solar neighbourhood: Galactic tidal perturbations". Monthly Notices of the Royal Astronomical Society. 430 (1): 403–415. arXiv:1212.4150. doi:10.1093/mnras/sts647.

[218] [218]
Giammichele, N.; Bergeron, P.; Dufour, P. (April 2012). "Know Your Neighborhood: A Detailed Model Atmosphere Analysis of Nearby White Dwarfs". The Astrophysical Journal Supplement. 199 (2): 35. arXiv:1202.5581. Bibcode:2012ApJS..199...29G. doi:10.1088/0067-0049/199/2/29. S2CID 118304737. 29.

[219] [219]
Delfosse, Xavier; et al. (April 1999). "New neighbours. I. 13 new companions to nearby M dwarfs". Astronomy and Astrophysics. 344: 897–910. arXiv:astro-ph/9812008. Bibcode:1999A&A...344..897D.

[1]

[2]

[3]

[4]

[5]

[6]

[7]

[8]

[9]

[10]

[11]

[12]

[13]

[14]

[15]

[16]

[17]

[18]

[19]

[20]

[21]

[22]

[23]

[24]

[25]

[26]

[27]

[28]

[29]

[30]

[31]

[32]

[33]

[34]

[35]

[36]

[37]

[38]

[39]

[40]

[41]

[42]

[43]

[44]

[45]

[46]

[47]

[48]

[49]

[50]

[51]

[52]

[53]

[54]

[55]

[56]

[57]

[58]

[59]

[60]

[61]

[62]

[63]

[64]

[65]

[66]

[67]

[68]

[69]

[70]

[71]

[72]

[73]

[74]

[75]

[76]

[77]

[78]

[79]

[80]

[81]

[82]

[83]

[84]

[85]

[86]

[87]

[88]

[89]

[90]

[91]

[92]

[93]

[94]

[95]

[96]

[97]

[98]

[99]

[100]

White dwarf

Mass–radius relationship

Radiation and cooling

Atmosphere and spectra

Metal-rich white dwarfs

Magnetic field

Stars with very low mass

Stars with low to medium mass

Stars with medium to high mass

Type Iax supernova

Type Ia supernovae

Post-common envelope binary

Cataclysmic variables

Other multiple-star systems

Wikiwand in your browser!

Discovery

Composition and structure

Variability

Formation

Fate

Debris disks and planets

Habitability

Binary stars and novae

Nearest

See also

References

External links and further reading