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.

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.

scholarly journals The evolution of massive binary systems

2020 ◽  
pp. 1-13
Author(s):  
Jelena Petrovic
Keyword(s):  
Binary Systems ◽  
Gamma Ray ◽  
Massive Stars ◽  
Compact Objects ◽  
Close Binary ◽  
Extensive Literature ◽  
Single Star ◽  
Close Binary Systems ◽  
Massive Binary Systems ◽  
Massive Close Binary

The evolution of massive stars in close binary systems is significantly different from single star evolution due to a series of interactions between the two stellar components. Such massive close binary systems are linked to various astrophysical phenomena, for example Wolf-Rayet stars, supernova type Ib and Ic, X-ray binaries and gamma-ray bursts. Also, the emission of gravitational waves, recently observed by the LIGO-Virgo detectors, is associated with mergers in binary systems containing compact objects, relics of massive stars - black holes and neutron stars. Evolutionary calculations of massive close binary systems were performed by various authors, but many aspects are not yet fully understood. In this paper, the main concepts of massive close binary evolution are reviewed, together with the most important parameters that can influence the final outcome of the binary system evolution, such as rotation, magnetic fields, stellar wind mass loss and mass accretion efficiency during interactions. An extensive literature overview of massive close binary models in the light of exciting observations connected with those systems is presented.

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.

scholarly journals Glimpses of Be Binary Evolution

2000 ◽  
Vol 175 ◽  
pp. 668-680 ◽  
Author(s):  
Douglas R. Gies
Keyword(s):  
Neutron Stars ◽  
Binary Systems ◽  
Rotational Velocity ◽  
Close Binary ◽  
Be Stars ◽  
Star System ◽  
Single Star ◽  
X Ray ◽  
Binary Evolution ◽  
X Ray Binaries

AbstractModels of close binary evolution predict that mass gainers will be spun up to speeds close to the critical rotational velocity while the mass donors will appear as stripped down He stars, white dwarfs, or neutron stars. I argue here that the mass gainers are closely related to the Be stars. I present a list of the known Be binary systems which consists of those with bright, Roche-filling companions and those with faint or undetected companions. Notably absent are Be + B systems which are expected if the Be phase is a stage in the life of a single star. We now have the first example of a Be + He star system in the binary, ϕ Per, and taken together with the well known Be X-ray binaries, there is clear evidence that some fraction of Be stars are created in binaries; whether all such rapid rotators are so formed remains unknown.

scholarly journals Stagnation-point flow in colliding-wind binary systems

1995 ◽  
Vol 163 ◽  
pp. 522-522
Author(s):  
Ian R. Stevens ◽  
Andrew M.T. Pollock
Keyword(s):  
Radiation Field ◽  
Binary Systems ◽  
Mass Loss Rate ◽  
Terminal Velocity ◽  
Close Binary ◽  
Single Star ◽  
Lower Velocity ◽  
X Ray ◽  
Radiation Fields ◽  
Star Models

The low X-ray temperatures and luminosities of colliding wind binaries compared to theoretical expectations has been a long standing problem. As a potential solution to this problem we present quantitative calculations of the radiation hydrodynamics in colliding wind binary systems, accounting for the effect of two radiation fields on the dynamics of both winds, using a formulation similar to that of Castor et al. (1975, ApJ 195, 157). A more detailed description of this work can be found in Stevens & Pollock (1994, MNRAS in press). Consider only the WR wind being driven under the influence of the WR and O-star radiation fields and motion only on the line-of-centers. Near the WR-star, its own radiation field dominates, and the mass-loss rate will be largely unaffected by the presence of the companion. However, moving towards the O-star, the O-star radiation field becomes a significant fraction of the total flux. As the O-star radiation field is opposed to the WR radiation field the radiative line-force will be diminished and the wind acceleration diminished. This will lead to the WR star wind colliding with the O-star wind at a lower velocity than would be expected from single star models. This mechanism will only be at work in close binary systems. In wide binaries both winds will be at terminal velocity before the other radiation field makes a difference. Results for a sample calculation are shown in Fig 1, using parameters for V444 Cyg from Schmutz et al. (1989, A&A 210, 236). In the absence of any deceleration effects the WR wind velocity at the shock would be ∼ 1300 km s−1, corresponding to kT ∼ 2 keV. The reduction in the WR star velocity at the shock interface caused by the O-star radiation field is predicted to be ∼ x2 leading to kTx ∼ 0.5 keV, in line with X-ray observations.

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
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