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Mass-ratio distribution of contact binary stars [PDF]
Astronomy & 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.
Milan Pešta, Ondřej Pejcha
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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, T. +9 more
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Contact tracing of binary stars: Pathways to stellar mergers [PDF]
Astronomy & 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 +2 more
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The light-curve intrinsic variability in 47 Kepler contact binary stars [PDF]
Monthly Notices of the Royal Astronomical Society, 2022 ABSTRACT This work studies the significance of light-curve intrinsic variability in the numerical modelling of contact binaries. Using synthetic light curves, we show that the starspot-based intrinsic variability increases the apparent mass ratio by $\Delta q=5{{\ \rm per\ cent}}$.
B. Debski
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Origin of the orbital period change in contact binary stars [PDF]
International Journal of Modern Physics E, 2019 The evolution of contact binary star systems in mass asymmetry (transfer) coordinate is considered. The orbital period changes are explained by an evolution in mass asymmetry towards the symmetry (symmetrization of binary system). It is predicted that decreasing and increasing orbital periods are related, respectively, with the nonoverlapping and ...
Sargsyan, V. V. +3 more
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A Cyclic Thermal Instability in Contact Binary Stars [PDF]
Symposium - International Astronomical Union, 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 ...
B. Flannery
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Masses and angular momenta of contact binary stars [PDF]
Monthly Notices of the Royal Astronomical Society: Letters, 2006 Abstract Results are presented on component masses and system angular momenta for over 100 low-temperature contact binaries. It is found that the secondary components in close binary systems are very similar in mass. Our observational evidence strongly supports the argument that the evolutionary process goes from near-contact binaries to
Gazeas, K.D., Niarchos, P.G.
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AROSATSurvey of Contact Binary Stars [PDF]
The Astronomical Journal, 2006 19 pages, 5 figures, accepted by ...
Geske, M. T. +2 more
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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 ...
S. Rucinski
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On the properties of contact binary stars [PDF]
Astronomy & Astrophysics, 2004 5 pages, 4 figures, accepted for publication in A& ...
Csizmadia, Sz., Klagyivik, P.
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