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Mass-ratio distribution of contact binary stars [PDF]
Astronomy and Astrophysics, 2023 The mass ratioqof a contact binary star evolves through mass transfer, magnetic braking, and thermal relaxation oscillations to low values until it crosses a critical thresholdqmin. When this occurs, the binary undergoes the tidal Darwin instability, leading to a rapid coalescence of the components and to an observable brightening of the system.
Ondřej Pejcha
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Contact tracing of binary stars: Pathways to stellar mergers [PDF]
Astronomy and Astrophysics, 2023 Stellar mergers are responsible for a wide variety of phenomena such as rejuvenated blue stragglers, highly magnetised stars, spectacular transients, iconic nebulae, and stars with peculiar surface chemical abundances and rotation rates. Before stars merge, they enter a contact phase.
J Henneco, F R N Schneider, E Laplace
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On the properties of contact binary stars [PDF]
Astronomy and Astrophysics, 2004 5 pages, 4 figures, accepted for publication in A& ...
Sz Csizmadia, P Klagyivik
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Study on the physical parameters of 18 contact binary stars
Monthly Notices of the Royal Astronomical SocietyABSTRACT We present the photometric light curve solutions of 18 W Ursae Majoris-type contact binary stars with orbital periods shorter than 0.5 d. This investigation utilized photometric data from the Transiting Exoplanet Survey Satellite, Gaia, and the All Sky Automated Survey for SuperNovae.
Átila Poro +2 more
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A Catalog of 1022 Bright Contact Binary Stars [PDF]
Astronomical Journal, 2006 In this work we describe a large new sample of contact binary stars extracted in a uniform manner from sky patrol data taken by the ROTSE-I telescope. Extensive ROTSE-I light curve data is combined with J, H, and K band near-infrared data taken from the Two Micron All-Sky Survey (2MASS) to add color information. Contact binaries candidates are selected
Timothy A Mckay
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A Cyclic Thermal Instability in Contact Binary Stars [PDF]
Astrophysical Journal, 1976 Contact binary stars coupled by a common convective envelope in which the entropy is constant, the Lucy model, are unstable against mass exchange: if either component begins to transfer mass, it will continue to do so. A detailed sequence of models is calculated which follows the thermal evolution of a 2M⊙ contact binary of normal Population I ...
Brian P Flannery
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Contact binary stars of the W UMa-type as distance tracers [PDF]
New Astronomy Reviews, 2004 IAU Sydney 2003, JD13 Extragalactic Binaries, ed.I.Ribas, uses elsart3 ...
Slavek M Rucinski
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Contact binary stars. I - an X-ray survey
Astrophysical Journal, 1984 X-ray emission from a contact binary star was first detected by the HEAO 1 satellite in 1977. Spectroscopic observations of 44i Boo and VW Cep by IUE established the presence of high-temperature chromospheric and transition region emission lines in the spectra of these stars.
R G Cruddace, A K Dupree
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Chromospheric activity in bright contact binary stars [PDF]
Astronomy & Astrophysics, 2020 Context. Studying chromospheric activity of contact binaries is an effective way of revealing the magnetic activity processes of these systems. One efficient but somewhat neglected method for this purpose is to follow the changes of the Hα line profiles via optical spectroscopy. Aims. Our goal is to perform a comprehensive preliminary analysis based on
Mitnyan Tibor +9 more
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ZZ Piscis Austrinus (ZZ PsA): a bright red nova progenitor and the instability mass ratio of contact binary stars [PDF]
Monthly Notices of the Royal Astronomical Society, 2020 ZZ Piscis Austrinus (ZZ PsA) is a neglected bright southern contact binary system with maximum V magnitude of 9.26. We present the first multiband photometric analysis and find the system to be in deep contact (>95 per cent) with an extremely low mass ...
Surjit S Wadhwa +2 more
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