| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Camelopardalis |
| Right ascension | 05h 22m 33.5306s[1] |
| Declination | +79° 13′ 52.143″[1] |
| Apparent magnitude (V) | 5.08[2] |
| Characteristics | |
| Spectral type | F7V[3] |
| U−B color index | −0.13 |
| B−V color index | 0.506±0.002[2] |
| Astrometry | |
| Radial velocity (Rv) | −11.09(13)[1] km/s |
| Proper motion (μ) | RA: −78.661(67) mas/yr[1] Dec.: 162.098(77) mas/yr[1] |
| Parallax (π) | 48.1098 ± 0.0727 mas[1] |
| Distance | 67.8 ± 0.1 ly (20.79 ± 0.03 pc) |
| Absolute magnitude (MV) | 3.59[4] |
| Details | |
| Mass | 1.29[5] M☉ |
| Radius | 1.51+0.02 −0.06[6] R☉ |
| Luminosity | 3.428±0.017[6] L☉ |
| Surface gravity (log g) | 4.22[5] cgs |
| Temperature | 6,396+135 −36[6] K |
| Metallicity [Fe/H] | 0.14[5] dex |
| Rotational velocity (v sin i) | 14.3[5] km/s |
| Age | 1.80[5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 33564 (K Camelopardalis) is a single[7] star with an exoplanetary companion in the northern constellation of Camelopardalis. It has an apparent visual magnitude of 5.08,[2] which means it is a 5th magnitude star that is faintly visible to the naked eye. The system is located at a distance of 68 light years from the Sun based on parallax, and it is drifting closer with a radial velocity of −11 km/s.[1] It is a candidate member of the Ursa Major Moving Group.[8]
This is an ordinary F-type main-sequence star with a stellar classification of F7V,[3] indicating that the star is hotter and more massive than the Sun, giving it a yellow-white hue. The star is about two[5] billion years old and is chromospherically quiet,[9] with a projected rotational velocity of 14.3 km/s. It has about 1.5[6] times the radius and 1.3[5] times the mass of the Sun. The star is radiating 3.4 times the luminosity of the Sun from its photosphere at an effective temperature of 6,396 K.[5]
Planetary system
In September 2005, a massive planet was found on an eccentric orbit about the star, based on radial velocity variations measured by the ELODIE spectrograph. An infrared excess had been detected at a wavelength of 60 μm, suggesting the star may host a circumstellar disk. However, the existence of a disk is unlikely because the infrared radiation is coming from a background galaxy.[9]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >9.1 MJ | 1.1 | 388 ± 3 | 0.34 ± 0.02 | — | — |
See also
References
- ^ a b c d e f Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
- ^ a b Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637. S2CID 119476992.
- ^ Huang, W.; et al. (2012). "A catalogue of Paschen-line profiles in standard stars". Astronomy & Astrophysics. 547: A62. arXiv:1210.7893. Bibcode:2012A&A...547A..62H. doi:10.1051/0004-6361/201219804. S2CID 119286159.
- ^ a b c d e f g h Luck, R. Earle (January 2017). "Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants". The Astronomical Journal. 153 (1): 19. arXiv:1611.02897. Bibcode:2017AJ....153...21L. doi:10.3847/1538-3881/153/1/21. S2CID 119511744. 21.
- ^ a b c d Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ Halbwachs, J. -L; et al. (2018). "Multiplicity among solar-type stars. IV. The CORAVEL radial velocities and the spectroscopic orbits of nearby K dwarfs". Astronomy and Astrophysics. 619: A81. arXiv:1808.04605. Bibcode:2018A&A...619A..81H. doi:10.1051/0004-6361/201833377. S2CID 119437322.
- ^ Montes, D.; et al. (November 2001). "Late-type members of young stellar kinematic groups - I. Single stars". Monthly Notices of the Royal Astronomical Society. 328 (1): 45–63. arXiv:astro-ph/0106537. Bibcode:2001MNRAS.328...45M. doi:10.1046/j.1365-8711.2001.04781.x. S2CID 55727428.
- ^ a b c Galland, F.; et al. (2005). "Extrasolar planets and brown dwarfs around A-F type stars II. A planet found with ELODIE around the F6V star HD 33564". Astronomy and Astrophysics. 444 (2): L21–L24. arXiv:astro-ph/0509112. Bibcode:2005A&A...444L..21G. doi:10.1051/0004-6361:200500176. S2CID 119341964.
External links
- "Notes for star HD 33564". Extrasolar Planets Encyclopaedia. Archived from the original on November 6, 2007. Retrieved 2008-08-20.
- HR%201686 HR 1686
- obswww.unige.ch
- CCDM J05227+7913
- Image HD 33564
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