Structure and evolution of large groups of Massive Close Binary systems

1982 ◽  
Vol 87 (1-2) ◽  
pp. 357-375 ◽  
Author(s):  
C. Doom ◽  
J. P. De Grève
Keyword(s):  
Binary Systems ◽  
Close Binary ◽  
Close Binary Systems ◽  
Large Groups ◽  
Massive Close Binary

Case a evolution of massive close binary systems

1987 ◽  
Vol 134 (1) ◽  
pp. 161-176 ◽  
Author(s):  
Masaomi Nakamura ◽  
Yasuhisa Nakamura
Keyword(s):  
Binary Systems ◽  
Close Binary ◽  
Close Binary Systems ◽  
Massive Close Binary

scholarly journals Apsidal motion in massive close binary systems – I. HD 165052, an extreme case?

2013 ◽  
Vol 433 (2) ◽  
pp. 1300-1311 ◽  
Author(s):  
G. Ferrero ◽  
R. Gamen ◽  
O. Benvenuto ◽  
E. Fernández-Lajús
Keyword(s):  
Binary Systems ◽  
Extreme Case ◽  
Close Binary ◽  
Apsidal Motion ◽  
Close Binary Systems ◽  
Massive Close Binary

scholarly journals Two Types of Evolution of Massive Close Binary Systems

1976 ◽  
Vol 73 ◽  
pp. 27-34 ◽  
Author(s):  
C. De Loore ◽  
J. P. De Greve
Keyword(s):  
Mass Exchange ◽  
Binary Systems ◽  
Supernova Explosion ◽  
Close Binary ◽  
Helium Burning ◽  
Primary Star ◽  
Close Binary Systems ◽  
First Case ◽  
Initial Chemical Composition ◽  
Massive Close Binary

It is well known that the outcome of case B evolution of the primaries of massive close binary systems (M1 ≥ 9 M⊙) depends on the initial primary mass. The most massive primaries finally ignite carbon, form iron cores and presumably end in a supernova explosion, whereas the lighter ones presumably end as white dwarfs, without carbon ignition. This paper derives an estimate of the mass boundary separating these two kinds of evolution.As an example of the first case, the evolution of a 20 M⊙ + 14 M⊙ system was computed; after the mass exchange, the primary star (with M = 5.43 M⊙) evolves through the helium-burning (Wolf-Rayet) stage towards a supernova explosion; finally the system evolves into an X-ray binary (BWRX-evolution).As a representative for the second case the evolution of a 10 M⊙ + 8 M⊙ system was examined. After the first stage of mass exchange, the primary (with a mass of 1.66 M⊙) approaches the helium main sequence; during later phases of helium burning the radius increases again, and a second stage of mass transfer starts; after this the star (with a mass of 1.14 M⊙) again evolves towards the left in the Hertzsprung-Russell diagram and ends as a white dwarf (BSWD-evolution). A system of 15 M⊙ + 8 M⊙ is found to evolve very similar to the 20 M⊙ + 14 M⊙ system. The mass Mu, separating the two types of evolution, must therefore be situated between 10 and 15 solar masses. An initial chemical composition X = 0.70, Z = 0.03 was used for all systems.

Case a evolution of massive close binary systems

1987 ◽  
Vol 134 (2) ◽  
pp. 219-234 ◽  
Author(s):  
Masaomi Nakamura ◽  
Yasuhisa Nakamura
Keyword(s):  
Binary Systems ◽  
Close Binary ◽  
Close Binary Systems ◽  
Massive Close Binary

scholarly journals Rotation and Massive Close Binary Evolution

2007 ◽  
Vol 3 (S250) ◽  
pp. 167-178 ◽  
Author(s):  
Norbert Langer ◽  
Matteo Cantiello ◽  
Sung-Chul Yoon ◽  
Ian Hunter ◽  
Ines Brott ◽  
...  
Keyword(s):  
Binary Systems ◽  
Close Binary ◽  
Single Star ◽  
Essential Ingredient ◽  
Critical Rotation ◽  
Close Binary Systems ◽  
Star Models ◽  
Binary Evolution ◽  
Massive Close Binary

AbstractWe review the role of rotation in massive close binary systems. Rotation has been advocated as an essential ingredient in massive single star models. However, rotation clearly is most important in massive binaries where one star accretes matter from a close companion, as the resulting spin-up drives the accretor towards critical rotation. Here, we explore our understanding of this process, and its observable consequences. When accounting for these consequences, the question remains whether rotational effects in massive single stars are still needed to explain the observations.

CaseA evolution of massive close binary systems

1984 ◽  
Vol 104 (2) ◽  
pp. 367-387 ◽  
Author(s):  
Masaomi Nakamura ◽  
Yasuhisa Nakamura
Keyword(s):  
Binary Systems ◽  
Close Binary ◽  
Close Binary Systems ◽  
Massive Close Binary

scholarly journals Structure and evolution of massive single stars and their relevance for close binary systems

1995 ◽  
Vol 163 ◽  
pp. 15-23
Author(s):  
Norbert Langer
Keyword(s):  
Binary Systems ◽  
Massive Stars ◽  
Close Binary ◽  
Single Star ◽  
Close Binary Systems ◽  
Massive Close Binary

Differences in the evolution of massive single stars and components of massive close binary systems are investigated. While for stars above the red supergiant luminosity limit, single star and case B primary evolution merge into a single scenario, large differences for less massive stars are demonstrated to occur at the example of MZAMS = 40M⊙, concerning the various WR subtypes, the nucleosynthesis yields, and the supernova stage.

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