Solar Physics

УРАВНЕНИЙ Мирнамик Мирахмедага оглы Баширов, кандидат физика математических наук, доцент НАН Азербайджана, Шамахинская Астрофизическая Обсерватория им.Насираддина Туси, Аннотация. Рассмотрена магнито-гидродинамическое (МГД) теория анизотропного солнечного ветра, с учетом тепловых поток и разности компонентов теплового давления. Исследованы радиальные зависимости скорости солнечного ветра, тепловых скоростей плазменных частиц от радиальной расстояние от солнца и асимптотика поведение этих параметров. Выявлено что сингулярность имеется в основном на расстояние до расстояние 8 радиуса Солнца от ее поверхности. Найдено что в данном рассмотрение число сингулярных точек имеется больше чем 3. И это связано тепловыми потоками которые учитывается в задаче. Асимптотические зависимости для скорости солнечного ветра и для компонентов теплового движение частиц солнечного ветра совпадает с зависимостями полученные численного вычисления. Зависимости и найденные частное решении дает представление об радиальном зависимости скорости ветра и результаты использованы при интерпретации получаемых энергии частицами, который позже ускоряются. Ключевые слова. МГД, солнечный ветер, корона, число Маха, гелиосфера

A superluminal quantum-vortex model of the electron and the positron is produced from a superluminal double-helix model of the photon during electron-positron pair production. The two oppositely-charged (with Q = ±e sqrt (2/α) = 16.6e) open-helix spin-½ half-photons compose the double-helix photon. These half-photons separate and curl up their separated superluminal single-helical trajectories to form an electrically-charged superluminal closed-helix spin-½ quantum-vortex electron model and a corresponding positron model. The helical radius and the Dirac equation's zitterbewegung angular frequency of the quantum vortex electron and positron models equal the helical radius and zitterbewegung angular frequency of the two spin-½ half-photons, each of energy E = mc^2 , that composed the double-helix photon model of energy E = 2mc^2 from which the electron and positron models were produced. The photon and electron models are also compatible when a photon of energy E > 2mc^2 produces a relativistic electron-positron pair. Implications of the quantum vortex electron model for electron stability are discussed.

We present multiwavelength observations of a large-amplitude oscillation of a polar crown filament on 15 October 2002. The oscillation occurred during the slow rise (about 1 km/s) of the filament. It completed three cycles before sudden acceleration and eruption. The oscillation and following eruption were clearly seen in observations recorded by the Extreme-Ultraviolet Imaging Telescope onboard SOHO. The oscillation was seen only in a part of the filament, and it appears to be a standing oscillation rather than a propagating wave. The period of oscillation was about two hours and did not change significantly during the oscillation. We also identified the oscillation as a "winking filament" in the H-alpha images taken by the Flare Monitoring Telescope, and as a spatial displacement in 17 GHz microwave images from Nobeyama Radio Heliograph (NoRH). The filament oscillation seems to be triggered by magnetic reconnection between a filament barb and nearby emerging magnetic flu...

During the studied period 1996-2007 I noticed that, the rising and oscillations of the sea level, global temperature, carbon dioxide concentration, ice mass of Antarctica, and melting of Greenland ice are highly correlated with Earth's orbital perturbations. Monthly variations of those parameters have two periodicities. Stronger one called “long-periodic cycle”, it is strongly related to solar activity. It appears as a rising trend during my studied period. Observation data of iceberg mass and its melting, global sea level, and concentration of greenhouse gases such as carbon dioxide is recent and does not cover a millennium or Wolf-Gleissberg solar cycle. So, it does not indicate a global warming. Second cycle is called “short-periodic cycle”. it is a weaker force but still stronger than human activities forcing. It appears as oscillations around the rising trend. The short periodic cycle of all mentioned parameters is found correlated to Earth's orbital perturbations which are indicating a global warming and global warming is a natural phenomenon. Global warming is strongly corelated to Sun, Earth’s orbit, and our  space.  I conclude that the productivity of natural greenhouse gases is greater than that produced by human activity. The current proposed global warming is not a result of human activities, rather just temporary epoch and natural phenomena. The Earth's orbital perturbations are in an excellent positive coherence with the Greenland ice mass but in a negative coherence with the Antarctic ice mass. My results are in good agreement with Yousef (2000) and Akasofu (2010).  I propose that the natural source of rising in concentration of greenhouse gases can be attributed to two causes: 1) Comets and asteroids, which are still carrying water molecules and some of greenhouse gas’ molecules to the Earth’s atmosphere; 2) Solar wind, which is composed greenhouse gases in ionization state. It may react and recombined though upper atmosphere before arriving to atmospheric lower levels at poles by unknown process. The global temperature is found to be correlated to Earth’s orbital perturbation too. This is because the declination angle is varying through the year. Output solar energy that arrives to the Earth depends on Sun-Earth distance too.

[Abstract is written mainly for fellow-scientists/researchers; Summary is more 'broad'.] In September 1859, the famous "Carrington Event" occurred (with estimated Dst readings of −850 nT to −900 nT), the largest recorded solar geomagnetic event since accurate records were made, causing widespread failures to contemporary telegraph systems and producing brilliant polar aurorae. In July 2012, a solar storm of much greater strength almost hit earth, narrowly missing because we'd moved about nine (9) days [about 2.46% of earth's 365¼−day orbit] from its trajectory[70], with a peak Dst value of −1,182 nT, as reported by Space Weather[31]. As a result, astronomers & scientists worldwide began calculating the probability estimation of another catastrophic Carrington−like geomagnetic event, since current technology (communications, GPS, power grids, satellites, etc.) are much more vulnerable to a severe solar storms than in the past when the only 'electronics' available were long−wire telegraphs-before even the telephone had been invented. Prior published research gave widely varying probability estimations of another such event. Moreover, prior research did not take into account the upcoming Maunder Minimum or acceleration in the geomagnetic pole movement, and the acceleration in the collapse of earth's protective magnetic field; nor, did they account for "lesser" magnetic storms which were very destructive, in their own right, causing many failures of communications and the power grid in various parts of the world. Historically, earth's magnetic north pole has wandered at a rate of about 0-15 km/year, but beginning in 1990, it accelerated to its current velocity of about 60 km/year[64] [65][66], which affects compasses, GPS, & other navigation. Moreover, the last time earth's protective magnetic field dropped by 30%, it needed fully 3,000 years[56], but, at the rapid rate it's decreasing now, it's projected to need only about 338.5 or 363.2 years (or 364.3 years or 333.9583 years), to drop by another 30%, depending of which set of data is used. While the data aren't in complete agreement, they're all very close, and suggest that a "geomagnetic flip," with concurrent field collapse to almost zero strength, is imminent. This is relevant because the weaker earth's protective magnetic field gets, the less it protects earth from severe geomagnetic storms. We review solar/geomagnetic data of all storms from the Carrington Event until present and estimate the probability of another similar catastrophic solar storm in the next decade: Prior prominent research of another Carrington Event are, at one extreme, Riley's estimates of about 12% probability[50], and Moriña's estimates[40] about 1.17% (taking the average of "0.46% and 1.88%," from his research paper). We find an 8.57% chance of another Carrington−class solar storm in the next decade. While we may overestimate the probabilities of another similar storm, the dangers posed to modern−day technology (much more vulnerable to geomagnetic solar storms or EMP detonations) suggest that it's better to use cautious & conservative estimates-especially given new unknowns and variables, such as the impending geomagnetic flip and concomitant collapse of earth's protective magnetic field-which, of course, make us even more vulnerable to a "direct hit." I stand by my estimate as it's methods are sound, with results between both extremes in the reported literature-and put forth proposed solutions for lawmakers and citizens.

In solar physics many questions remain unanswered, such as the solar coronal heating problem in the solar atmosphere or magnetic field generation in the solar interior. However, there is a growing consensus that many different physical phenomena will combine to give a solution to these problems.
From the solar coronal heating point of view, one possible phenomenon to study is resonant absorption, which allows the natural transfer of wave energy to and from the background plasma. If the plasma is dissipative this energy can be converted into heat. One of the stumbling blocks when studying resonant absorption is that linear theory can breakdown around the resonant point. This causes a dilemma: use linear theory as an approximation regardless to try and find sensible solutions or try and solve the difficult, but realistic, nonlinear equations.
The present thesis will investigate the nonlinearity associated with resonant absorption. There are two different resonances in solar plasmas, one is the Alfve ́n resonance and the other is the slow resonance. Previous studies, in nonlinear theory, have concentrated mainly on the slow resonances as they are more affected by nonlinearity. We will study both the Alfve ́n and the slow resonances. The present thesis will analytically investigate these resonances in anisotropic, dispersive and dissipative plasmas - typical conditions of the solar upper atmosphere.
The second manifestation of nonlinearity is the generation of a mean shear flow outside the layer enclosing the resonant surface. We will derive the governing equations for this gener- ated flow at the Alfve ́n resonance. These flows (like all flows) are completely determined by the boundary conditions and we produce an example flow.
The thesis culminates by studying coupled resonances; when the distance between an Alfve ́n and slow resonance is so small (in comparison to the incoming wave) they act as if they interact with an incoming wave simultaneously. We derive the governing equations for the absorption of fast magnetoacoustic waves at the coupled resonance, and then numerically analyse the coeffi- cient of wave energy absorption to compare with the results found for single resonances. We find that the absorption of fast magnetoacoustic waves is far more efficient under coronal conditions compared with chromospheric conditions despite an increase in absorption due to the coupled resonance.

The general apologetic theme of this study was to highlight the actions that had been taken to assure, protect and guide the birth of Jesus Christ.  Bible study practices of scrutinizing New Testament scriptures carrying the words “behold,” “lo” or “see” was introduced.  A percentage of those three English words had been translated from the Greek words ίδε (IDE) and ίδου (IDOU).  Since they had served as Active and Middle Voices, respectively, for the two Imperative Mood verbs, they were used as study markers.  Summaries of various contextual analyses and the results of epifluorescent confocal laser scanning microscopy of papyrus fragments served as indicators of the historical reliability of the Gospels by Matthews and Luke.  Justifications for expecting the relatively warm winter background of the Nativity was based on the effects of the Roman Solar Maximum.  The shortcomings of astronomical and astrological hypotheses were compared with the strengths of the Shekinah Glory and growing legitimacy of UFOs as explanations for the Star of Bethlehem for the Star of Bethlehem.

The Square Kilometre Array (SKA) will be the largest radio telescope ever built, aiming to provide collecting area larger than 1 km 2. The SKA will have two independent instruments, SKA-LOW comprising of dipoles organized as aperture arrays in Australia and SKA-MID comprising of dishes in South Africa. Currently the phase-1 of SKA, referred to as SKA1, is in its late design stage and construction is expected to start in 2020. Both SKA1-LOW (frequency range of 50-350 MHz) and SKA1-MID Bands 1, 2, and 5 (frequency ranges of 350-1050, 950-1760, and 4600-15300 MHz, respectively) are important for solar observations. In this paper we present SKA's unique capabilities in terms of spatial, spectral, and temporal resolution, as well as sensitivity and show that they have the potential to provide major new insights in solar physics topics of capital importance including (i) the structure and evolution of the solar corona, (ii) coronal heating, (iii) solar flare dynamics including particle acceleration and transport, (iv) the dynamics and structure of coronal mass ejections, and (v) the solar aspects of space weather. Observations of the Sun jointly with the new generation of ground-based and space-borne instruments promise unprecedented discoveries.

The solar flare and Coronal Mass Ejections (CMEs) are well known as one of the most massive
eruptions which potentially create major disturbances in the interplanetary medium and initiate severe
magnetic storms when they collide with the Earth‟s magnetosphere. However, how far the solar flare
can contribute to the formation of the CMEs is still not easy to be understood. These phenomena are
associated with II and III burst it also divided by sub-type of burst depending on the physical
characteristics and different mechanisms. In this work, we used a Compound Astronomical Low-cost
Low-frequency Instrument for Spectroscopy in Transportable Observatories (CALLISTO) system.
The aim of the present study is to reveal dynamical properties of solar burst type II and III due to
several mechanisms. Most of the cases of both solar radio bursts can be found in the range less that
400 MHz. Based on solar flare monitoring within 24 hours, the CMEs that has the potential to explode
will dominantly be a class of M1 solar flare. Overall, the tendencies of SRBT III burst form the solar
radio burst type III at 187 MHz to 449 MHz. Based on solar observations, it is evident that the
explosive, short time-scale energy release during flares and the long term, gradual energy release
expressed by CMEs can be reasonably understood only if both processes are taken as common and
probably not independent signatures of a destabilization of pre-existing coronal magnetic field
structures. The configurations of several active regions can be sourced regions of CMEs formation.
The study of the formation, acceleration and propagation of CMEs requires advanced and powerful
observational tools in different spectral ranges as many „stages‟ as possible between the photosphere
of the Sun and magnetosphere of the Sun and magnetosphere of the Earth. In conclusion, this range is
a current regime of solar radio bursts during CMEs events.

The fields of solar radiophysics and solar system radio physics, or radio heliophysics, will benefit immensely from an instrument with the capabilities projected for SKA. Potential applications include interplanetary scintillation (IPS), radio-burst tracking, and solar spectral radio imaging with a superior sensitivity. These will provide breakthrough new insights and results in topics of fundamental importance, such as the physics of impulsive energy releases, magnetohydrodynamic oscillations and turbulence, the dynamics of post-eruptive processes, energetic particle acceleration , the structure of the solar wind and the development and evolution of solar wind transients at distances up to and beyond the orbit of the Earth. The combination of the high spectral, time and spatial resolution and the unprecedented sensitivity of the SKA will radically advance our understanding of basic physical processes operating in solar and heliospheric plasmas and provide a solid foundation for the forecasting of space weather events. Advancing Astrophysics with the Square Kilometre Array

We have analyzed the stand-off distance values of 101 interplanetary CMEs (ICMEs) observed during the
period 1997–2005. Main aim of the present work is to study the stand-off distance and its dependence
on various parameters of CMEs, ICMEs and IPshocks, Alfvenic Mach numbers and transit time. From the
distribution, the stand-off time and stand-off distance values of many of the events are found to be in the
range between
2–20 hand
1–40 R (R Solar radius). From the correlation between speed of CMEs
and stand-off distance, we noted smaller stand-off distance for energetic CMEs, which indicated that
the driver CME (CME which is generating the shock) and its shock travel closely together. From the
correlation plot between CME acceleration and stand-off distance, we found that the highly decelerated
events and highly accelerated events have lower stand-off distance range (i.e.,10–40 R) than the other
events. The events with longer travel time to reach 1AU (470 h) show stand-off times r20 h and for
those faster events (VCME42200km/s) with smaller travel time (r40 h), stand-off time is extremely low
(r10h). A wide range of stand-off distance is seen for a particular value of CME and ICME parameters.
The poor correlations of stand-off distance with all the above parameters confirm that the stand-off
distance does not strongly depend on CME, ICME and IPshock parameters, but depends on a
combination of all these parameters. On the other hand, the faster CMEs having lower stand-off distance
and/or stand-off time imply that as long as the CMEs are energetic, the CMEs and shocks travel closely
together. Also, it can be noted that the stand-off distance is not only dependent on gamma, but it is
related to other parameters.

The Sun's electron number density profile ne(r) is not well measured and understood from the Sun's photosphere (r = RS) to the solar wind (say, r > 10 RS), despite its great importance for solar physics. A powerful new technique is developed and applied to extract ne(r) directly from the time-varying frequency of coronal type III radio bursts, for the first time. Unexpectedly, wind-like regions with ne = A (r - RS)-2 are common below 2RS, and coronal type III bursts often are almost linear in 1/f - t dynamic spectra. Indices lower and higher than 2 also occur, the former plausibly due to non-radial curved magnetic field lines. The profile ne = A (r - RS)-2 is consistent with the coronal radio data, type III simulations, and previous models based on eclipse and coronagraph observations. It gives a first physical basis for the previous models. A simple interpretation is in terms of conical flow from localized sources close to the photosphere, plausibly corresponding to UV f...

The SOHO mission has achieved important results in the physics of solar wind and coronal mass ejection acceleration, but most of the processes that drive this acceleration have not yet been explained. The Advanced Spectroscopic and Coronagraphic Explorer (ASCE) mission will carry on-board spectroscopic and polarimetric instrumentation of new generation that is designed to address the fundamental questions on this processes. Following a brief description of ASCE scientific objectives and instrumentation, the EUV polarimetric channel is described. The EUV Polarimeter (EUVP) is designed to measure for the first time the magnetic field vector in the extended corona through the Hanle effect, and the anisotropy of the ion velocity. The EUVP represents the contribution of the Italian solar physics community to the ASCE mission.

This paper discusses the advance of the speleothem luminescence
research.  Potential,  resolution  and  limitations  of  high  resolution  luminescence  speleothem  proxy  records  of
Paleotemperature, Solar Insolation, Solar Luminosity, Glaciations, Sea Level advances, Past Precipitation, Plants
Populations, Paleosoils, Past Karst Denudation, Chemical Pollution, Cosmic Rays Flux variations, Cosmogenic
Isotopes production and Supernova Eruptions in the Past, Advances of Hydrothermal Waters, and Techtonic Uplift are
discussed. It is demonstrated that speleothems allow extremely high resolution (higher than in any other paleoclimatic
terrestrial archives) and long duration of records. Some speleothems can be used as natural climatic stations for
obtaining of quantitative proxy records of Quaternary climates with annual resolution.

Solar radio emission features a large number of fine structures demonstrating great variability in frequency and time. We present spatially resolved spectral radio observations of type IIIb bursts in the 30 − 80 MHz range made by the Low Frequency Array (LOFAR). The bursts show well-defined fine frequency structuring called "stria" bursts. The spatial characteristics of the stria sources are determined by the propagation effects of radio waves; their movement and expansion speeds are in the range of (0.1−0.6)c. Analysis of the dynamic spectra reveals that both the spectral bandwidth and the frequency drift rate of the striae increase with an increase of their central frequency; the striae bandwidths are in the range of ∼ (20 − 100) kHz and the striae drift rates vary from zero to ∼ 0.3 MHz s −1. The observed spectral characteristics of the stria bursts are consistent with the model involving modulation of the type III burst emission mechanism by small-amplitude fluctuations of the plasma density along the electron beam path. We estimate that the relative amplitude of the density fluctuations is of ∆n/n ∼ 10 −3 , their characteristic length scale is less than 1000 km, and the characteristic propagation speed is in the range of 400 − 800 km s −1. These parameters indicate that the observed fine spectral structures could be produced by propagating magnetohydrodynamic waves.