The evolutionary state of contact and near-contact binary stars

1988 ◽  
Vol 231 (2) ◽  
pp. 341-352 ◽  
Author(s):  
R. W. Hilditch ◽  
D. J. King ◽  
T. M. McFarlane
Keyword(s):  
Binary Stars ◽  
Evolutionary State ◽  
Contact Binary Stars ◽  
Contact Binary

scholarly journals On the properties of contact binary stars

2004 ◽  
Vol 426 (3) ◽  
pp. 1001-1005 ◽  
Author(s):  
Sz. Csizmadia ◽  
P. Klagyivik
Keyword(s):  
Binary Stars ◽  
Contact Binary Stars ◽  
Contact Binary

scholarly journals A Cyclic Thermal Instability in Contact Binary Stars

1976 ◽  
Vol 73 ◽  
pp. 331-331
Author(s):  
Brian P. Flannery
Keyword(s):  
Mass Exchange ◽  
Binary Stars ◽  
Thermal Evolution ◽  
Normal Population ◽  
Equal Mass ◽  
General Nature ◽  
Convective Envelope ◽  
Short Period ◽  
Contact Binary Stars ◽  
Contact Binary

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 abundances (X=0.70, Z = 0.02), starting at nearly equal mass. The initial instability develops into a cyclic mass-exchange with the mass fraction oscillating between 0.56≤m2/(m1 + m2)≤0.62 with a period of ~107yr. Throughout the cycle the component stars are not in thermal equilibrium. The instability is of a general nature, and such oscillating systems can satisfactorily populate the short period, red region of the period color relation for WUMa stars.

scholarly journals Origin of the orbital period change in contact binary stars

2019 ◽  
Vol 28 (06) ◽  
pp. 1950044 ◽  
Author(s):  
V. V. Sargsyan ◽  
H. Lenske ◽  
G. G. Adamian ◽  
N. V. Antonenko
Keyword(s):  
Orbital Period ◽  
Binary Stars ◽  
Binary Systems ◽  
Binary Star ◽  
Period Change ◽  
Mass Asymmetry ◽  
Contact Binary Stars ◽  
Contact Binary ◽  
Energy Formula ◽  
Orbital Periods

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 overlapping stage of the binary star during its symmetrization. A huge amount of energy [Formula: see text][Formula: see text]J is converted from the potential energy into internal energy of the stars during the symmetrization. As shown, the merger of stars in the binary systems, including KIC 9832227, is energetically an unfavorable process. The sensitivity of the calculated results to the values of total mass and orbital angular momentum is analyzed.

scholarly journals AROSATSurvey of Contact Binary Stars

2006 ◽  
Vol 131 (1) ◽  
pp. 633-637 ◽  
Author(s):  
M. T. Geske ◽  
S. J. Gettel ◽  
T. A. McKay
Keyword(s):  
Binary Stars ◽  
Contact Binary Stars ◽  
Contact Binary

Contact binary stars. I - an X-ray survey

1984 ◽  
Vol 277 ◽  
pp. 263 ◽  
Author(s):  
R. G. Cruddace ◽  
A. K. Dupree
Keyword(s):  
Binary Stars ◽  
X Ray ◽  
Contact Binary Stars ◽  
Contact Binary

Gas–Dynamical Features of the Envelopes of Contact Binary Stars

2017 ◽  
Vol 61 (12) ◽  
pp. 1038-1043
Author(s):  
V. I. Shematovich ◽  
P. V. Kaigorodov ◽  
D. V. Bisikalo ◽  
A. M. Fateeva
Keyword(s):  
Binary Stars ◽  
Contact Binary Stars ◽  
Contact Binary ◽  
Dynamical Features
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