Results 1 to 10 of about 3,920 (285)
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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On the properties of contact binary stars [PDF]
Astronomy and Astrophysics, 2004 5 pages, 4 figures, accepted for publication in A& ...
Szilárd Csizmadia, P Klagyivik
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Contact tracing of binary stars: Pathways to stellar mergers [PDF]
Astronomy and AstrophysicsStellar 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.
Fabian Schneider +2 more
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Study on the physical parameters of 18 contact binary stars [PDF]
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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Absolute Dimensions of Contact Binary Stars in Baade Window [PDF]
Journal of Astronomy and Space Sciences, 1999 The light curves of the representative 6 contact binary stars observed by OGLE Project of searching for dark matter in our Galaxy have been analyzed by the method of the Wilson and Devinney Differential Correction to find photometric solutions.
Young Woon Kang
doaj +3 more sources
Minimum mass ratio of contact binary stars [PDF]
, 2022 Mass ratio $q$ of a contact binary star evolves due to mass transfer, magnetic braking, and thermal relaxation oscillations to small values until it crosses a critical threshold $q_\text{min}$. When that happens, the binary undergoes the tidal Darwin instability leading to a rapid coalescence of the components and observable brightening of the system ...
Milan Pešta, Ondřej Pejcha
openaire +2 more sources
Small Mass Ratio Contact Binary GR Vir and HV Aqr [PDF]
Journal of Astronomy and Space Sciences, 2004 The absolute dimensions of low mass contact binary, GR Vir and HV Aqr were obtained using WD program from the published spectroscopic and photometric observational data.
Kyu-Dong Oh +4 more
doaj +3 more sources
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 Mckay
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Low Mass Ratio Contact Binary V410 Aur and V776 Cas - II [PDF]
Journal of Astronomy and Space Sciences, 2005 New BVR CCD light curves of the low mass ratio contact binaries, V410 Aur and V776 Cas, were observed with the 61 cm reflector and a 2K CCD camera at the Sobaeksan Astronomical Observatory.
Kyu-Dong Oh, Chun-Hwey Kim, Ho-iL Kim
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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 Flannery
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