Conservative mass transfer in close binary systems. I - Equations of motion for spin and orbital angular momenta

1983 ◽  
Vol 266 ◽  
pp. 776 ◽  
Author(s):  
J. J. Matese ◽  
D. P. Whitmire
Keyword(s):  
Mass Transfer ◽  
Binary Systems ◽  
Equations Of Motion ◽  
Close Binary ◽  
Close Binary Systems ◽  
Angular Momenta

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 Evolutionary computations for intermediate mass close binary systems

1981 ◽  
Vol 59 ◽  
pp. 503-506
Author(s):  
Th. J. van der Linden
Keyword(s):  
Mass Transfer ◽  
Numerical Simulations ◽  
Binary Systems ◽  
Close Binary ◽  
Close Binaries ◽  
Intermediate Mass ◽  
Evolutionary Computations ◽  
Primary Mass ◽  
Close Binary Systems ◽  
Mass Ratios

AbstractNumerical simulations of the evolution of close binaries with primary mass between 3 and 15 Mʘ and mass ratios of ~ 1.5 were carried out. These results show that after mass transfer the system consists of a bright main-sequence.star together with a faint He-star in a rather wide orbit (p> 60d) Evolution of this kind predicts isotope anomalies for the CNO-elements with respect to their solar values.

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