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Contact Tracing of Massive Binary Stars
Proceedings of the International Astronomical Union, 2022AbstractStellar mergers produce more massive, rejuvenated (strongly magnetic) stars, with potentially peculiar properties, and can be detected as luminous red novae. Using a grid of detailed 1D binary evolution models, we aim to determine which binary systems are likely to merge and at what evolutionary stage.
Jan Henneco +3 more
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V0644 Ser: An Active Ultrashort Period Contact Binary Star
Research in Astronomy and Astrophysics, 2022Abstract The photometric solutions of the ultrashort period close binary V0644 Ser based on our new complete BVRI light curves are derived by the Wilson–Devininney code. The results show that V0644 Ser is a W-type shallow contact binary, and the third light was found in the
Hu-Shan Xu +3 more
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Close-in companions to contact binary stars
EAS Publications Series, 2013W UMa-type contact binaries are composed of two late-type main-sequence stars, where both components are filling their critical Roche Lobes and sharing a common convective envelope. Their formation and evolution are unsolved problems in stellar astrophysics. This kind of binary systems have the lowest angular momentum and shortest orbital periods among
S.B. Qian +5 more
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The evolutionary state of contact and near-contact binary stars
Monthly Notices of the Royal Astronomical Society, 1988Calcul des masses, rayons et luminosites des composantes de 31 systemes binaires de type F-K proches ou en ...
R. W. Hilditch +2 more
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Multiplicity of Contact Binary Stars
2007We present results of a preliminary investigation of triple star incidence for contact binary stars. The goal is to shed light on the possible role of distant companions which may have acquired and/or absorbed AM during evolution of multiple systems facilitating or enabling formation of contact binaries.
T. Pribulla, S.M. Rucinski
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KIC 4762887: A near-contact binary or an ellipsoidal variable star?
New Astronomy, 2021Abstract KIC 4762887 is a variable star with a very small amplitude discovered by K e p l e r and show the EW-type light curve. We analyzed the light curve of KIC 4762887 by using the 2015 version of the Wilson-Devinney code. The results indicated that it is not a contact binary, maybe not even an eclipsing binary.
Xu-Zhi Li, Liang Liu
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1990
A group of close binary stars named near-contact binaries is defined. They are divided according to their physical characteristics into to two subclasses: V1010 Ophiuchi binaries and FO Virginis binaries. A list of members of the group, their current observational status, and their physical and evolutionary relationship to W Ursa-Majoris binaries is ...
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A group of close binary stars named near-contact binaries is defined. They are divided according to their physical characteristics into to two subclasses: V1010 Ophiuchi binaries and FO Virginis binaries. A list of members of the group, their current observational status, and their physical and evolutionary relationship to W Ursa-Majoris binaries is ...
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Gas–Dynamical Features of the Envelopes of Contact Binary Stars
Astronomy Reports, 2017The results of three-dimensional numerical simulations of the gaseous envelope of a contact binary star with parameters similar to those of SV Cen are presented. The outflow of matter from the vicinity of the Lagrange point L2 leads to the formation of a disk-like common envelope with a radius of order three times the component separation.
V. I. Shematovich +3 more
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Updated catalogue of the light curve solutions of contact binary stars
Astronomische Nachrichten, 2007AbstractThe catalogue of the light curve solutions of contact binary stars was updated. Based on the catalogue data we call the attention to a remarkable gap in the temperature distribution of contact binaries which remained unexplained. The absolute dimensions of the components were calculated in a reliable way. (© 2007 WILEY‐VCH Verlag GmbH & Co.
Sz. Csizmadia +3 more
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Observational Evidence for the Evolution of Contact Binary Stars
1985This paper reviews data relevant to the evolution of contact binary stars. Statistics, photometric surveys, period changes and the results of light curve fitting are reviewed. These data are then compared with evolutionary models.
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