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Galaxies
Special Issues
New Insights on Binary Stars
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New Insights on Binary Stars

A special issue of Galaxies (ISSN 2075-4434).

Deadline for manuscript submissions: closed (20 December 2022) | Viewed by 9451

Special Issue Editors

Prof. Dr. Ronald Mennickent

E-Mail Website
Guest Editor
Department of Astronomy, University of Concepción, Concepción 4030000, Chile
Interests: binary stars; close binary stars; interacting binary stars; Be stars; mass flows and accretion disks in binaries; binary star evolution; variable stars; chromospherically active stars; transient phenomena; luminous blue variables; massive stars
Prof. Dr. Anatoly Miroshnichenko

E-Mail Website
Guest Editor
Department of Physics and Astronomy, University of North Carolina Greensboro, Greensboro, NC 27412, USA
Interests: circumstellar matter; binary systems; radiative transfer
Special Issues, Collections and Topics in MDPI journals
Dr. Vitaly Neustroev

E-Mail Website
Guest Editor
Space Physics and Astronomy Research Unit, University of Oulu, 90570 Oulu, Finland
Interests: interacting binary stars (cataclysmic variables and low-mass X-ray binaries); accretion discs; transient phenomena; time series analysis; image processing; computational astrophysics

Special Issue Information

Dear Colleagues,

Large-scale astronomical surveys and satellite data provide new opportunities for the study of binary stars. State-of-the-art technology, mosaic-based and fast detectors, as well as continuous or regular observational cadences permit the study of binary stars at new scales of the time domain and at an unprecedented level of precision. This Special Issue of Galaxies titled "New insights on binary stars" is open to fresh and novel research articles on binary stars aiming to gain knowledge on different aspects of binary stars in the context of stellar populations, as well as in the framework of binary star evolution. This includes systems with different orbit sizes and with stellar components of different masses, including systems with compact and non-compact objects. Dedicated studies on binary star interaction and circumstellar matter are also encouraged.

Prof. Dr. Ronald Mennickent
Prof. Dr. Anatoly Miroshnichenko
Dr. Vitaly Neustroev
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. Galaxies is an international peer-reviewed open access semimonthly journal published by MDPI.

Please visit the Instructions for Authors page before submitting a manuscript. The Article Processing Charge (APC) for publication in this open access journal is 1400 CHF (Swiss Francs). 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

  • stellar astrophysics
  • binary stars
  • binary star evolution
  • stellar populations
  • binaries with compact objects
  • close interacting binaries
  • stellar-size accretion disks
  • binary star evolution

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Published Papers (4 papers)

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Research

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27 pages, 1325 KiB  
Article
Searching for Phase-Locked Variations of the Emission-Line Profiles in Binary Be Stars
by Anatoly S. Miroshnichenko, Raghav Chari, Stephen Danford, Peter Prendergast, Alicia N. Aarnio, Ivan L. Andronov, Lidiia L. Chinarova, Aidan Lytle, Ainash Amantayeva, Ilfa A. Gabitova, Nadezhda L. Vaidman, Sayat S. Baktybayev and Serik A. Khokhlov
Galaxies 2023, 11(4), 83; https://doi.org/10.3390/galaxies11040083 - 4 Jul 2023
Cited by 4 | Viewed by 2149
Abstract
There is growing evidence that many Be stars are parts of binary systems. As the B-type primaries are very fast rotators and their spectral lines may be distorted by the circumstellar material, it is not easy to measure their radial velocity directly from [...] Read more.
There is growing evidence that many Be stars are parts of binary systems. As the B-type primaries are very fast rotators and their spectral lines may be distorted by the circumstellar material, it is not easy to measure their radial velocity directly from the spectral lines. It has been shown that some Be binaries exhibit peak intensity variations consisting of double-peaked Hα lines that are phase-locked with orbital periods. We searched for such variations in the spectra of 12 Be stars, including several known and suspected binaries. Our results include confirmation of the orbital periods in ν Geminorum, ϵ Capricorni, κ Draconis, 60 Cygni, and V2119 Cygni, its refinement in o Puppis, as well as suggesting hints for binarity in o Aquarii, BK Camelopardalis, and 10 Cassiopeae. Monitoring of the Hα line profile variations in β Canis Minoris for over the last 10 years gives further support to the existence of a 182.5-day period found earlier in a smaller set of data. A similar but still preliminary period (179.6 days) was found in the Hα line profile variations in ψ Persei. It is shown for the first time that ν Geminorum exhibits phase-locked variations in the Hα emission peak intensity ratio and, therefore, is a part of the inner binary in this triple system. Our results show that the mentioned phase-locked peak intensity variations are observed in more Be binary systems than previously known and can be used to search for binarity of Be stars when application of other methods is inconclusive. Full article
(This article belongs to the Special Issue New Insights on Binary Stars)
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12 pages, 2741 KiB  
Article
Refining Orbits of Bright Binary Systems
by Anatoly S. Miroshnichenko, Stephen Danford, Ivan L. Andronov, Alicia N. Aarnio, Duncan Lauer and Holly Buroughs
Galaxies 2023, 11(1), 8; https://doi.org/10.3390/galaxies11010008 - 31 Dec 2022
Cited by 3 | Viewed by 2084
Abstract
We obtained spectra of several bright binary systems (ζ02 UMa, 2 Lac, and ϕ Aql), which were mostly observed with photographic plates and whose orbits were not determined very accurately. Each system was monitored for a few years with the 81-cm [...] Read more.
We obtained spectra of several bright binary systems (ζ02 UMa, 2 Lac, and ϕ Aql), which were mostly observed with photographic plates and whose orbits were not determined very accurately. Each system was monitored for a few years with the 81-cm telescope equipped with an échelle spectrograph at the Three College Observatory in North Carolina. The spectra were taken in a wavelength range between 4000 and 7900 Å with a spectral resolution of R∼ 12,000. Radial velocity measurements were done using cross-correlation in selected spectral regions or by measuring positions of individual spectral lines. Refined orbits and stellar parameters are presented. Full article
(This article belongs to the Special Issue New Insights on Binary Stars)
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38 pages, 6701 KiB  
Article
MHD Modeling of Mass Transfer Processes in Close Binary Stars
by Andrey Zhilkin, Andrey Sobolev and Dmitry Bisikalo
Galaxies 2022, 10(6), 110; https://doi.org/10.3390/galaxies10060110 - 5 Dec 2022
Cited by 1 | Viewed by 1902
Abstract
A three-dimensional numerical model has been developed to study the flow structure in close binary systems with a magnetic field. The model uses a system of equations of modified magnetic hydrodynamics, which allows describing all the main dynamic effects associated with the magnetic [...] Read more.
A three-dimensional numerical model has been developed to study the flow structure in close binary systems with a magnetic field. The model uses a system of equations of modified magnetic hydrodynamics, which allows describing all the main dynamic effects associated with the magnetic field. It takes into account the processes of radiation heating and cooling, heating due to current dissipation, as well as magnetic field diffusion. The model allows calculations in a wide range of magnetic field values. Comparison of the calculation results with observational data confirms the reliability and high efficiency of the model. The paper presents the calculation results of the flow structure in a typical intermediate polar. It is shown that an accretion disk is formed in such a binary system, which has the following characteristic features: “hot line”, tidal shock waves, precession density wave, magnetospheric region, and accretion columns. In this case, the magnetic field in the disk is predominantly toroidal. The paper also presents the results of calculations for typical polars. In such systems, instead of an accretion disk, a collimated stream of matter is formed, moving along the magnetic field lines to the magnetic poles of the white dwarf. It is shown that in synchronous polars, variations of the mass transfer rate lead to a change in the spatial configuration of the flow. In asynchronous polars, changes in the flow structure for different phases of the beat period are observed as well as the processes of switching the flow between the magnetic poles of the accretor. Numerical calculations of the asynchronous system are performed under the assumption of the dipole configuration of the magnetic field for different values of the dipole offset relative to the center of the white dwarf. The paper presents a method for estimating this offset from observational light curves. Full article
(This article belongs to the Special Issue New Insights on Binary Stars)
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Review

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19 pages, 719 KiB  
Review
Recent Progress in Finding Binary Systems with the B[e] Phenomenon
by Anatoly S. Miroshnichenko, Sergei V. Zharikov, Nadine Manset, Serik A. Khokhlov, Atilkhan S. Nodyarov, Valentina G. Klochkova, Stephen Danford, Aizhan K. Kuratova, Ronald Mennickent, S. Drew Chojnowski, Ashish Raj and Devendra Bisht
Galaxies 2023, 11(1), 36; https://doi.org/10.3390/galaxies11010036 - 17 Feb 2023
Cited by 3 | Viewed by 2135
Abstract
This paper describes recent studies of the FS CMa-type objects, a group of stars showing the B[e] phenomenon defined in 2007. The objects exhibit strong emission-line spectra with both permitted and forbidden lines suggesting the presence of a B-type star as well as [...] Read more.
This paper describes recent studies of the FS CMa-type objects, a group of stars showing the B[e] phenomenon defined in 2007. The objects exhibit strong emission-line spectra with both permitted and forbidden lines suggesting the presence of a B-type star as well as strong IR excesses due to radiation of circumstellar dust. These properties are hard to explain in the framework of the evolution of single stars with luminosities between ~300 and ~30,000 L⊙ typical of most B-type stars. We explore the hypothesis that the gaseous-and-dusty envelopes of FS CMa objects are due to either earlier or ongoing mass transfer between the binary system components. It is hard to detect the secondary components in these systems because of veiling and distortions by the circumstellar matter because of the relative faintness of the companions. Nevertheless, we detected regular radial velocity variations of the spectral lines in MWC 728, 3 Pup, and AS 386 and we found absorption lines typical of cool stars in the spectra of MWC 645, AS 174, and several other objects. The diversity of the secondary components in FS CMa objects is discussed in the context of non-conservative binary evolution. Full article
(This article belongs to the Special Issue New Insights on Binary Stars)
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