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Advances in the Physics of Stars - in Memory of...
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Advances in the Physics of Stars - in Memory of Prof. Yuri N. Gnedin

A special issue of Universe (ISSN 2218-1997). This special issue belongs to the section "Galaxies and Clusters".

Deadline for manuscript submissions: closed (31 December 2021) | Viewed by 25251

Printed Edition Available!
A printed edition of this Special Issue is available here.

Special Issue Editors

Prof. Dr. Nazar R. Ikhsanov

E-Mail Website
Guest Editor
Pulkovo Observatory of the Russian Academy of Sciences, 196140 Saint Petersburg, Russia
Interests: astrophysics
Prof. Dr. Galina L. Klimchitskaya

E-Mail Website
Guest Editor
1. Pulkovo Observatory of the Russian Academy of Sciences, 196140 Saint Petersburg, Russia
2. Peter the Great Saint Petersburg Polytechnic University, 195251 Saint Petersburg, Russia
Interests: astrophysics; atomic physics; condensed matter physics
Special Issues, Collections and Topics in MDPI journals
Prof. Dr. Vladimir M. Mostepanenko

E-Mail Website
Guest Editor
1. Pulkovo Observatory of the Russian Academy of Sciences, 196140 Saint Petersburg, Russia
2. Peter the Great Saint Petersburg Polytechnic University, 195251 Saint Petersburg, Russia
Interests: astrophysics; cosmology; quantum field theory
Special Issues, Collections and Topics in MDPI journals

Special Issue Information

Dear Colleagues,

This Special Issue will collect articles devoted to all aspects of the physics of stars and galaxies, including an investigation of their types, properties, stages of evolution, and distribution in the Universe. It is devoted to the memory of outstanding scientist Prof. Dr. Yuri N. Gnedin who not only organized the Department of Astrophysics at Pulkovo Astronomical Observatory of the Russian Academy of Sciences and led it for several decades, but also initiated a number of prospective research projects in several other astrophysical institutions. The scope of scientific interests and expertise of Prof. Gnedin were extraordinarily wide. He produced pioneering works in the theoretical description of polarized radiation transfer, generation of high-energy radiation in tight binary star systems and galactic nuclei, cyclotron lines in spectra of accreting neutron stars, determination of magnetic fields of cosmic sources from polarimetric observations, physics of intermediate-mass and supermassive black holes and magnetic white dwarfs, supernovae, exoplanets and dark satellites of stars, cosmic gamma-ray bursts, dark matter and dark energy. Both observational and theoretical aspects of the above and some other subjects will be covered in this Special Issue, which will contain research as well as review articles.

Prof. Dr. Nazar R. Ikhsanov
Prof. Dr. Galina L. Klimchitskaya
Prof. Dr. Vladimir M. Mostepanenko
Guest Editors

Manuscript Submission Information

Manuscripts should be submitted online at www.mdpi.com by registering and logging in to this website. Once you are registered, click here to go to the submission form. Manuscripts can be submitted until the deadline. All submissions that pass pre-check are peer-reviewed. Accepted papers will be published continuously in the journal (as soon as accepted) and will be listed together on the special issue website. Research articles, review articles as well as short communications are invited. For planned papers, a title and short abstract (about 100 words) can be sent to the Editorial Office for announcement on this website.

Submitted manuscripts should not have been published previously, nor be under consideration for publication elsewhere (except conference proceedings papers). All manuscripts are thoroughly refereed through a single-blind peer-review process. A guide for authors and other relevant information for submission of manuscripts is available on the Instructions for Authors page. Universe is an international peer-reviewed open access monthly journal published by MDPI.

Please visit the Instructions for Authors page before submitting a manuscript. Submitted papers should be well formatted and use good English. Authors may use MDPI's English editing service prior to publication or during author revisions.

Keywords

  • stars
  • black holes
  • neutron stars
  • white dwarfs
  • gamma-ray bursts
  • galactic nuclei
  • supernovae
  • radiation transfer
  • exoplanets
  • dark matter
  • dark energy

Published Papers (13 papers)

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Editorial

Jump to: Research, Review

5 pages, 697 KiB  
Editorial
Editorial to the Special Issue “Advances in the Physics of Stars—In Memory of Prof. Yuri N. Gnedin”
by Nazar R. Ikhsanov, Galina L. Klimchitskaya and Vladimir M. Mostepanenko
Universe 2022, 8(4), 239; https://0-doi-org.brum.beds.ac.uk/10.3390/universe8040239 - 13 Apr 2022
Viewed by 1668
Abstract
This Special Issue collects articles devoted to various aspects of astrophysics which can be understood as a science investigating stars, galaxies, their types and properties, stages of their evolution, distribution in the Universe and the interstellar and intergalactic media [...] Full article
(This article belongs to the Special Issue Advances in the Physics of Stars - in Memory of Prof. Yuri N. Gnedin)
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Research

Jump to: Editorial, Review

8 pages, 2900 KiB  
Article
Remembering Yury N. Gnedin at the Dawn of X-ray Polarimetry: Predictions of IXPE Observations of Neutron Stars
by Jeremy Heyl
Universe 2022, 8(2), 84; https://0-doi-org.brum.beds.ac.uk/10.3390/universe8020084 - 28 Jan 2022
Cited by 2 | Viewed by 1999
Abstract
NASA’s Imaging X-ray Polarimetry Explorer (IXPE) was launched in December 2021. It is 100 times more sensitive to polarized X-ray emission than any preceding mission and it is opening a new observational window into high-energy astrophysics. I outline Yury N. Gnedin’s many contributions [...] Read more.
NASA’s Imaging X-ray Polarimetry Explorer (IXPE) was launched in December 2021. It is 100 times more sensitive to polarized X-ray emission than any preceding mission and it is opening a new observational window into high-energy astrophysics. I outline Yury N. Gnedin’s many contributions to understanding polarization from neutron stars and present new simulations of observations that IXPE will perform of the X-ray pulsar Hercules X-1 and the magnetar 4U 0141+561 in February 2022. These observations highlight and test particular models that Gnedin and collaborators first proposed. I outline how IXPE will provide unique constraints on the structure and kinematics of the boundary region between the accretion flow and the neutron star surface of Hercules X-1 and how IXPE will verify the predictions of vacuum birefringence for the magnetar 4U 0142+561. Full article
(This article belongs to the Special Issue Advances in the Physics of Stars - in Memory of Prof. Yuri N. Gnedin)
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10 pages, 778 KiB  
Article
On the Origin of Persistent Radio and X-ray Emission from Brown Dwarf TVLM 513-46546
by Alexander Stepanov and Valery Zaitsev
Universe 2022, 8(2), 77; https://0-doi-org.brum.beds.ac.uk/10.3390/universe8020077 - 27 Jan 2022
Cited by 4 | Viewed by 1543
Abstract
We study the origin of unusually persistent microwave and X-ray radiation from the ultracool dwarf TVLM 513-46546. It is shown that the source of ≈1 keV X-ray emission is not the entire corona of the brown dwarf, but a population of several hundreds [...] Read more.
We study the origin of unusually persistent microwave and X-ray radiation from the ultracool dwarf TVLM 513-46546. It is shown that the source of ≈1 keV X-ray emission is not the entire corona of the brown dwarf, but a population of several hundreds of coronal magnetic loops, with 10 MK plasma heated upon dissipation of the electric current generated by the photospheric convection. Unlike models, which assume a large-scale magnetic structure of the microwave source, our model suggests that the microwave radiation comes from hundreds of magnetic loops quasi-uniformly distributed over the dwarf’s surface. We propose a long-term operating mechanism of acceleration of electrons generating gyrosynchrotron radio emission caused by oscillations of electric current in the magnetic loops as an equivalent RLC circuit. The second population of magnetic loops—the sources of microwave radiation, is at the same time a source of softer (≈0.2 keV) X-ray emission. Full article
(This article belongs to the Special Issue Advances in the Physics of Stars - in Memory of Prof. Yuri N. Gnedin)
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24 pages, 1694 KiB  
Article
Particle Acceleration in Mildly Relativistic Outflows of Fast Energetic Transient Sources
by Andrei Bykov, Vadim Romansky and Sergei Osipov
Universe 2022, 8(1), 32; https://0-doi-org.brum.beds.ac.uk/10.3390/universe8010032 - 05 Jan 2022
Cited by 4 | Viewed by 2578
Abstract
Recent discovery of fast blue optical transients (FBOTs)—a new class of energetic transient sources—can shed light on the long-standing problem of supernova—long gamma-ray burst connections. A distinctive feature of such objects is the presence of modestly relativistic outflows which place them in between [...] Read more.
Recent discovery of fast blue optical transients (FBOTs)—a new class of energetic transient sources—can shed light on the long-standing problem of supernova—long gamma-ray burst connections. A distinctive feature of such objects is the presence of modestly relativistic outflows which place them in between the non-relativistic and relativistic supernovae-related events. Here we present the results of kinetic particle-in-cell and Monte Carlo simulations of particle acceleration and magnetic field amplification by shocks with the velocities in the interval between 0.1 and 0.7 c. These simulations are needed for the interpretation of the observed broad band radiation of FBOTs. Their fast, mildly to moderately relativistic outflows may efficiently accelerate relativistic particles. With particle-in-cell simulations we demonstrate that synchrotron radiation of accelerated relativistic electrons in the shock downstream may fit the observed radio fluxes. At longer timescales, well beyond those reachable within a particle-in-cell approach, our nonlinear Monte Carlo model predicts that protons and nuclei can be accelerated to petaelectronvolt (PeV) energies. Therefore, such fast and energetic transient sources can contribute to galactic populations of high energy cosmic rays. Full article
(This article belongs to the Special Issue Advances in the Physics of Stars - in Memory of Prof. Yuri N. Gnedin)
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43 pages, 14653 KiB  
Article
Multi-Component MHD Model of Hot Jupiter Envelopes
by Andrey Zhilkin and Dmitri Bisikalo
Universe 2021, 7(11), 422; https://0-doi-org.brum.beds.ac.uk/10.3390/universe7110422 - 05 Nov 2021
Cited by 9 | Viewed by 2179
Abstract
A numerical model description of a hot Jupiter extended envelope based on the approximation of multi-component magnetic hydrodynamics is presented. The main attention is focused on the problem of implementing the completed MHD stellar wind model. As a result, the numerical model becomes [...] Read more.
A numerical model description of a hot Jupiter extended envelope based on the approximation of multi-component magnetic hydrodynamics is presented. The main attention is focused on the problem of implementing the completed MHD stellar wind model. As a result, the numerical model becomes applicable for calculating the structure of the extended envelope of hot Jupiters not only in the super-Alfvén and sub-Alfvén regimes of the stellar wind flow around and in the trans-Alfvén regime. The multi-component MHD approximation allows the consideration of changes in the chemical composition of hydrogen–helium envelopes of hot Jupiters. The results of calculations show that, in the case of a super-Alfvén flow regime, all the previously discovered types of extended gas-dynamic envelopes are realized in the new numerical model. With an increase in magnitude of the wind magnetic field, the extended envelope tends to become more closed. Under the influence of a strong magnetic field of the stellar wind, the envelope matter does not move along the ballistic trajectory but along the magnetic field lines of the wind toward the host star. This corresponds to an additional (sub-Alfvénic) envelope type of hot Jupiters, which has specific observational features. In the transient (trans-Alfvén) mode, a bow shock wave has a fragmentary nature. In the fully sub-Alfvén regime, the bow shock wave is not formed, and the flow structure is shock-less. Full article
(This article belongs to the Special Issue Advances in the Physics of Stars - in Memory of Prof. Yuri N. Gnedin)
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10 pages, 266 KiB  
Communication
Cosmological Model with Interconnection between Dark Energy and Matter
by Gennady S. Bisnovatyi-Kogan
Universe 2021, 7(11), 412; https://0-doi-org.brum.beds.ac.uk/10.3390/universe7110412 - 29 Oct 2021
Cited by 4 | Viewed by 1022
Abstract
It is accepted in the present cosmology model that the scalar field, which is responsible for the inflation stage in the early universe, transforms completely into matter, and the accelerated universe expansion is presently governed by dark energy (DE), whose origin is not [...] Read more.
It is accepted in the present cosmology model that the scalar field, which is responsible for the inflation stage in the early universe, transforms completely into matter, and the accelerated universe expansion is presently governed by dark energy (DE), whose origin is not connected with the inflationary scalar field. We suppose here that dark matter (DM) has a common origin with a small variable component of dark energy (DEV). We suggest that DE may presently have two components, one of which is the Einstein constant Λ, and another, smaller component DEV (ΛV) comes from the remnants of the scalar field responsible for inflation, which gave birth to the origin of presently existing matter. In this note we consider only the stages of the universe expansion after recombination, z≃1100, when DM was the most abundant component of the matter, therefore we suggest for simplicity that a connection exists between DM and DEV so that the ratio of their densities remains constant over all the stages after recombination, ρDM=αρDEV, with a constant α. One of the problems revealed recently in cosmology is a so-called Hubble tension (HT), which is the difference between values of the present Hubble constant, measured by observation of the universe at redshift z≲1, and by observations of a distant universe with CMB fluctuations originated at z∼1100. In this paper we suggest that this discrepancy may be explained by deviation of the cosmological expansion from a standard Lambda-CDM model of a flat universe, due to the action of an additional variable component DEV. Taking into account the influence of DEV on the universe’s expansion, we find the value of α that could remove the HT problem. In order to maintain the almost constant DEV/DM energy density ratio during the time interval at z<1100, we suggest the existence of a wide mass DM particle distribution. Full article
(This article belongs to the Special Issue Advances in the Physics of Stars - in Memory of Prof. Yuri N. Gnedin)
17 pages, 1233 KiB  
Article
A Simple Model of Radiation from a Magnetized Neutron Star: Accreted Matter and Polar Hotspots
by Dmitry Yakovlev
Universe 2021, 7(11), 395; https://0-doi-org.brum.beds.ac.uk/10.3390/universe7110395 - 21 Oct 2021
Cited by 1 | Viewed by 1261
Abstract
A simple and well known model for thermal radiation spectra from a magnetized neutron star is further studied. The model assumes that the star is internally isothermal and possesses a dipole magnetic field (B≲1014 G) in the outer heat-insulating [...] Read more.
A simple and well known model for thermal radiation spectra from a magnetized neutron star is further studied. The model assumes that the star is internally isothermal and possesses a dipole magnetic field (B≲1014 G) in the outer heat-insulating layer. The heat transport through this layer makes the surface temperature distribution anisotropic; any local surface element is assumed to emit a blackbody (BB) radiation with a local effective temperature. It is shown that this thermal emission is nearly independent of the chemical composition of insulating envelope (at the same taken averaged effective surface temperature). Adding a slight extra heating of magnetic poles allows one to be qualitatively consistent with observations of some isolated neutron stars. Full article
(This article belongs to the Special Issue Advances in the Physics of Stars - in Memory of Prof. Yuri N. Gnedin)
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16 pages, 994 KiB  
Article
Dark Matter Axions, Non-Newtonian Gravity and Constraints on Them from Recent Measurements of the Casimir Force in the Micrometer Separation Range
by Galina L. Klimchitskaya and Vladimir M. Mostepanenko
Universe 2021, 7(9), 343; https://0-doi-org.brum.beds.ac.uk/10.3390/universe7090343 - 12 Sep 2021
Cited by 9 | Viewed by 1668
Abstract
We consider axionlike particles as the most probable constituents of dark matter, the Yukawa-type corrections to Newton’s gravitational law and constraints on their parameters following from astrophysics and different laboratory experiments. After a brief discussion of the results by Prof. Yu. N. Gnedin [...] Read more.
We consider axionlike particles as the most probable constituents of dark matter, the Yukawa-type corrections to Newton’s gravitational law and constraints on their parameters following from astrophysics and different laboratory experiments. After a brief discussion of the results by Prof. Yu. N. Gnedin in this field, we turn our attention to the recent experiment on measuring the differential Casimir force between Au-coated surfaces of a sphere and the top and bottom of rectangular trenches. In this experiment, the Casimir force was measured over an unusually wide separation region from 0.2 to 8μm and compared with the exact theory based on first principles of quantum electrodynamics at nonzero temperature. We use the measure of agreement between experiment and theory to obtain the constraints on the coupling constant of axionlike particles to nucleons and on the interaction strength of a Yukawa-type interaction. The constraints obtained on the axion-to-nucleon coupling constant and on the strength of a Yukawa interaction are stronger by factors of 4 and 24, respectively, than those found previously from gravitational experiments and measurements of the Casimir force but weaker than the constraints following from a differential measurement where the Casimir force was nullified. Some other already performed and planned experiments aimed at searching for axions and non-Newtonian gravity are discussed, and their prospects are evaluated. Full article
(This article belongs to the Special Issue Advances in the Physics of Stars - in Memory of Prof. Yuri N. Gnedin)
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15 pages, 1099 KiB  
Communication
Determination of the Magnetic Field Strength and Geometry in the Accretion Disks of AGNs by Optical Spectropolarimetry
by Mikhail Piotrovich, Stanislava Buliga and Tinatin Natsvlishvili
Universe 2021, 7(6), 202; https://0-doi-org.brum.beds.ac.uk/10.3390/universe7060202 - 18 Jun 2021
Cited by 4 | Viewed by 1411
Abstract
Based on the spectropolarimetric data of 33 Seyfert type 1 galaxies observed with the BTA-6m telescope of the Special Astrophysical Observatory, we estimated the magnetic field values at the event horizon of the supermassive black hole BH and the exponents of the [...] Read more.
Based on the spectropolarimetric data of 33 Seyfert type 1 galaxies observed with the BTA-6m telescope of the Special Astrophysical Observatory, we estimated the magnetic field values at the event horizon of the supermassive black hole BH and the exponents of the power-law dependence s of the magnetic field on the radius. We used the model of optically thick geometrically thin Shakura–Sunyaev accretion disk. The average value of logBH[G] was found to be ∼4, which is in good agreement with the results obtained by other methods. The average value of s is s≈1.7, and its distribution maximum span is in the range od 1.85<s<2.0. This is a rather interesting result, since s=5/4 is usually adopted in calculations for Shakura–Sunyaev accretion disks. In addition, for two objects PG 1545+210 and 2MASX J06021107+2828382, the measured degree of polarization is greater than the maximum possible value at the angle between the line of sight and the axis of the accretion disk i=45°. It was concluded that for these objects the angle should be closer to i=60°. Full article
(This article belongs to the Special Issue Advances in the Physics of Stars - in Memory of Prof. Yuri N. Gnedin)
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Review

Jump to: Editorial, Research

12 pages, 331 KiB  
Review
Scattered Radiation of Protoplanetary Disks
by Vladimir P. Grinin and Larisa V. Tambovtseva
Universe 2022, 8(4), 224; https://0-doi-org.brum.beds.ac.uk/10.3390/universe8040224 - 02 Apr 2022
Cited by 3 | Viewed by 1568
Abstract
Scattered radiation of circumstellar (CS) dust plays an important role in the physics of young stars. Its observational manifestations are various but more often they are connected with the appearance of intrinsic polarization in young stars and their CS disks. In our brief [...] Read more.
Scattered radiation of circumstellar (CS) dust plays an important role in the physics of young stars. Its observational manifestations are various but more often they are connected with the appearance of intrinsic polarization in young stars and their CS disks. In our brief review we consider two classes of astrophysical objects in which the participation of scattered radiation is key for understanding their nature. First of all, these are irregular variables (UX Ori type stars). The modern idea of their nature and the mechanism of their variability has been formed thanks to synchronous observations of their linear polarization and brightness. The second class of objects is the CS disks themselves. Their detailed investigation became possible due to observations in polarized light using a coronographic technique and large telescopes. Full article
(This article belongs to the Special Issue Advances in the Physics of Stars - in Memory of Prof. Yuri N. Gnedin)
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10 pages, 310 KiB  
Review
Progress in Understanding the Nature of SS433
by Anatol Cherepashchuk
Universe 2022, 8(1), 13; https://0-doi-org.brum.beds.ac.uk/10.3390/universe8010013 - 27 Dec 2021
Cited by 2 | Viewed by 2685
Abstract
SS433 is the first example of a microquasar discovered in the Galaxy. It is a natural laboratory for studies of extraordinarily interesting physical processes that are very important for the relativistic astrophysics, cosmic gas dynamics and theory of evolution of stars. The object [...] Read more.
SS433 is the first example of a microquasar discovered in the Galaxy. It is a natural laboratory for studies of extraordinarily interesting physical processes that are very important for the relativistic astrophysics, cosmic gas dynamics and theory of evolution of stars. The object has been studied for over 40 years in the optical, X-ray and radio bands. By now, it is generally accepted that SS433 is a massive eclipsing X-ray binary in an advanced stage of evolution in the supercritical regime of accretion on the relativistic object. Intensive spectral and photometric observations of SS433 at the Caucasian Mountain Observatory of the P. K. Sternberg Astronomical Institute of M. V. Lomonosov Moscow State University made it possible to find the ellipticity of the SS433 orbit and to discover an increase in the system’s orbital period. These results shed light on a number of unresolved issues related to SS433. In particular, a refined estimate of the mass ratio MxMv>0.8 was obtained (Mx and Mv are the masses of the relativistic object and optical star). Based on these estimates, the relativistic object in the SS433 system is the black hole; its mass is >8M⊙. The ellipticity of the orbit is consistent with the “slaved” accretion disc model. The results obtained made it possible to understand why SS433 evolves as the semi-detached binary instead of the common envelope system. Full article
(This article belongs to the Special Issue Advances in the Physics of Stars - in Memory of Prof. Yuri N. Gnedin)
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16 pages, 4015 KiB  
Review
Searching for Magnetospheres around Herbig Ae/Be Stars
by Mikhail Pogodin, Natalia Drake, Nina Beskrovnaya, Sergei Pavlovskiy, Swetlana Hubrig, Markus Schöller, Silva Järvinen, Olesya Kozlova and Ilya Alekseev
Universe 2021, 7(12), 489; https://0-doi-org.brum.beds.ac.uk/10.3390/universe7120489 - 12 Dec 2021
Cited by 4 | Viewed by 1900
Abstract
We describe four different approaches for the detection of magnetospheric accretion among Herbig Ae/Be stars with accretion disks. Studies of several unique objects have been carried out. One of the objects is the Herbig Ae star HD 101412 with a comparatively strong magnetic [...] Read more.
We describe four different approaches for the detection of magnetospheric accretion among Herbig Ae/Be stars with accretion disks. Studies of several unique objects have been carried out. One of the objects is the Herbig Ae star HD 101412 with a comparatively strong magnetic field. The second is the early-type Herbig B6e star HD 259431. The existence of a magnetosphere in these objects was not recognized earlier. In both cases, a periodicity in the variation of some line parameters, originating near the region of the disk/star interaction, has been found. The third object is the young binary system HD 104237, hosting a Herbig Ae star and a T Tauri star. Based on the discovery of periodic variations of equivalent widths of atmospheric lines in the spectrum of the primary, we have concluded that the surface of the star is spotted. Comparing our result with an earlier one, we argue that these spots can be connected with the infall of material from the disk onto the stellar surface through a magnetosphere. The fourth example is the Herbig Ae/Be star HD 37806. Signatures of magnetospheric accretion in this object have been identified using a different method. They were inferred from the short-term variability of the He i λ5876 line profile forming in the region of the disk/star interaction. Full article
(This article belongs to the Special Issue Advances in the Physics of Stars - in Memory of Prof. Yuri N. Gnedin)
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21 pages, 366 KiB  
Review
Studies of Magnetic Chemically Peculiar Stars Using the 6-m Telescope at SAO RAS
by Iosif Romanyuk
Universe 2021, 7(12), 465; https://0-doi-org.brum.beds.ac.uk/10.3390/universe7120465 - 29 Nov 2021
Cited by 3 | Viewed by 1581
Abstract
We present a survey of the most important results obtained in observations with the 6-m telescope in the studies of magnetic fields of chemically peculiar stars. It is shown that we have found more than 200 new magnetic chemically peculiar stars, which is [...] Read more.
We present a survey of the most important results obtained in observations with the 6-m telescope in the studies of magnetic fields of chemically peculiar stars. It is shown that we have found more than 200 new magnetic chemically peculiar stars, which is more than 30% of their total known number. Observations of ultra-slow rotators (stars with rotation periods of years and decades) have shown that there are objects with strong fields among them, several kG in magnitude. In the association of young stars in Orion, it has been found that the occurrence and strength of magnetic fields of chemically peculiar stars decrease sharply with age in the interval from 2 to 10 Myr. These data indicate the fossil nature of magnetic fields of chemically peculiar stars. About 10 magnetic stars were found based on ultra-accurate photometry data obtained from the Kepler and TESS satellites. A new effective method of searching for magnetic stars was developed. In addition, the exact rotation periods make it possible to build reliable curves of the longitudinal field component variability with the phase of the star’s rotation period, and hence to create its magnetic model. The survey is dedicated to the memory of Prof. Yuri Nikolaevich Gnedin. Full article
(This article belongs to the Special Issue Advances in the Physics of Stars - in Memory of Prof. Yuri N. Gnedin)
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