Dynamical evolution of stellar orbits in close binary systems with conservative mass transfer

2008 ◽  
Vol 52 (8) ◽  
pp. 680-692 ◽  
Author(s):  
L. G. Luk’yanov
Keyword(s):  
Mass Transfer ◽  
Binary Systems ◽  
Dynamical Evolution ◽  
Close Binary ◽  
Stellar Orbits ◽  
Close Binary Systems

Close binary systems before and after mass transfer

1982 ◽  
Vol 87 (1-2) ◽  
pp. 377-401 ◽  
Author(s):  
F. Vansina ◽  
J. P. De Grève
Keyword(s):  
Mass Transfer ◽  
Binary Systems ◽  
Close Binary ◽  
Close Binary Systems ◽  
Before And After

scholarly journals Pulsars and Close Binary Systems

1971 ◽  
Vol 46 ◽  
pp. 273-278
Author(s):  
Virginia Trimble ◽  
Martin Rees
Keyword(s):  
Mass Transfer ◽  
Neutron Stars ◽  
Binary Systems ◽  
Alternative Explanation ◽  
Galactic Plane ◽  
Orbital Motion ◽  
Close Binary ◽  
Close Binaries ◽  
Close Binary Systems ◽  
Supernova Explosions

It is first considered what must happen if pulsars (i.e. neutron stars) are formed in close binary systems (CBS), and whether the resulting orbital motion and mass transfer should be observable. As this set of alternatives seems unlikely, there follow suggestions of how one might prevent the formation of neutron stars in close binaries. Finally, it is shown that ‘runaway’ pulsars with velocities larger than about 15 km/sec cannot be produced by isotropic supernova explosions within close binaries, and an alternative explanation is suggested for the observed correlation of periods of pulsars with their distances from the galactic plane.

scholarly journals Mass loss from interacting close binary systems

1981 ◽  
Vol 59 ◽  
pp. 431-456
Author(s):  
Mirek J. Plavec
Keyword(s):  
Mass Transfer ◽  
Mass Loss ◽  
Binary Stars ◽  
Binary Systems ◽  
Close Binary ◽  
Important Process ◽  
Close Binary Systems ◽  
Complex Process ◽  
General Complex ◽  
Mass Outflow

AbstractMass outflow from interacting close binary systems, accompanied by loss of orbital angular momentum, appears to be a very important process affecting the evolution of binary stars. Together with accretion on the mass-gaining component, it is the least understood aspect of the general complex process we call “evolution with mass transfer and/or mass loss”, or, more briefly, “interaction”. It is therefore very imperative to assemble and examine all available facts or hints about mass loss.

scholarly journals How galaxies form: Mass assembly from chemical abundances in the era of large surveys

2009 ◽  
Vol 5 (S265) ◽  
pp. 461-469
Author(s):  
Rosemary F.G. Wyse
Keyword(s):  
Mass Transfer ◽  
Large Scale ◽  
Binary Systems ◽  
Milky Way ◽  
Dynamical Evolution ◽  
Close Binary ◽  
Chemical Abundances ◽  
Milky Way Galaxy ◽  
Deep Imaging ◽  
Mass Assembly

AbstractThe chemical abundances in the atmosphere of a star provide unique information about the gas from which that star formed, and, modulo processes that are not important for the vast majority of stars, such as mass transfer in close binary systems, are conserved through a star's life. Correlations between chemistry and kinematics have been used for decades to trace dynamical evolution of the Milky Way Galaxy. I discuss how it should be possible to refine and extend such analyses, provided planned large-scale deep imaging surveys have matched spectroscopic surveys.

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