On the influence of mass loss and convective overshooting on the evolution of massive stars

Massevitch, A. G.; Popova, E. I.; Тутуков, А. В.; Yungelson, L. R.

doi:10.1007/bf00645480

Cited by 26 publications

(14 citation statements)

References 14 publications

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“…We emphasize that the above-described scenario applies only to close binaries, that have components massive enough to produce ECSN or core-collapse SN, but not so massive that the loss of the hydrogen envelope by stellar wind and an associated widening of the orbit via the Jeans mode of mass ejection may prevent RLOF by the primary. This limits the relevant mass range by M 1 ≲ (40–50) M ⊙ [470, 807]. …”

Section: Evolutionary Scenario For Compact Binaries With Neutron Starmentioning

confidence: 99%

The Evolution of Compact Binary Star Systems

Постнов

Yungelson

2014

Living Rev. Relativ.

461

382

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We review the formation and evolution of compact binary stars consisting of white dwarfs (WDs), neutron stars (NSs), and black holes (BHs). Mergings of compact-star binaries are expected to be the most important sources for forthcoming gravitational-wave (GW) astronomy. In the first part of the review, we discuss observational manifestations of close binaries with NS and/or BH components and their merger rate, crucial points in the formation and evolution of compact stars in binary systems, including the treatment of the natal kicks, which NSs and BHs acquire during the core collapse of massive stars and the common envelope phase of binary evolution, which are most relevant to the merging rates of NS-NS, NS-BH and BH-BH binaries. The second part of the review is devoted mainly to the formation and evolution of binary WDs and their observational manifestations, including their role as progenitors of cosmologically-important thermonuclear SN Ia. We also consider AM CVn-stars, which are thought to be the best verification binary GW sources for future low-frequency GW space interferometers.

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Section: Evolutionary Scenario For Compact Binaries With Neutron Starmentioning

confidence: 99%

The Evolution of Compact Binary Star Systems

Постнов

Yungelson

2014

Living Rev. Relativ.

461

382

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“…[1] Overshooting refers to a chemically mixed region beyond the boundary of the convective core (e.g. Maeder and Meynet, 1991;Massevitch et al, 1979;Stothers, 1963), as predicted by basic stellar evolutionary theory, i.e. the Schwarzschild criterion.…”

Section: Single Stellar Evolutionmentioning

confidence: 99%

The evolution of hierarchical triple star-systems

2016

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Field stars are frequently formed in pairs, and many of these binaries are part of triples or even higher-order systems. Even though, the principles of single stellar evolution and binary evolution, have been accepted for a long time, the long-term evolution of stellar triples is poorly understood. The presence of a third star in an orbit around a binary system can significantly alter the evolution of those stars and the binary system. The rich dynamical behaviour in three-body systems can give rise to Lidov-Kozai cycles, in which the eccentricity of the inner orbit and the inclination between the inner and outer orbit vary periodically. In turn, this can lead to an enhancement of tidal effects (tidal friction), gravitational-wave emission and stellar interactions such as mass transfer and collisions. The lack of a self-consistent treatment of triple evolution, including both three-body dynamics as well as stellar evolution, hinders the systematic study and general understanding of the long-term evolution of triple systems. In this paper, we aim to address some of these hiatus, by discussing the dominant physical processes of hierarchical triple evolution, and presenting heuristic recipes for these processes. To improve our understanding on hierarchical stellar triples, these descriptions are implemented in a public source code TrES, which combines three-body dynamics (based on the secular approach) with stellar evolution and their mutual influences. Note that modelling through a phase of stable mass transfer in an eccentric orbit is currently not implemented in TrES, but can be implemented with the appropriate methodology at a later stage.

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“…High mass transfers from the O-star occur only when it nearly fills its Roche Lobe. It is then bright for a time (Massevich et al , 1979) τ = 2.7 × 10 5 yr . (3.8) so the expected number of strong X-ray emitting binaries in the galaxy is…”

Section: Rate Of Formationmentioning

confidence: 99%

Contribution Of High-Mass Black Holes To Mergers Of Compact Binaries

2003

World Scientific Series in 20th Century Physics

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On the influence of mass loss and convective overshooting on the evolution of massive stars

Cited by 26 publications

References 14 publications

The Evolution of Compact Binary Star Systems

The Evolution of Compact Binary Star Systems

The evolution of hierarchical triple star-systems

Contribution Of High-Mass Black Holes To Mergers Of Compact Binaries

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