Evolution of massive close binaries and formation of neutron stars and black holes

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

doi:10.1007/bf00651192

Cited by 53 publications

(16 citation statements)

References 12 publications

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“…The scenario of the evolution of massive binaries from a pair of main-sequence stars to a relativistic binary consisting of NSs or BHs produced by core-collapse SN was independently elaborated by Tutukov and Yungelson [782, 472]20 and van den Heuvel et al [801, 201]. This scenario is fully confirmed by more than 30 years of astronomical observations and is now considered as “standard”.…”

Section: Evolutionary Scenario For Compact Binaries With Neutron Starmentioning

confidence: 99%

The Evolution of Compact Binary Star Systems

Постнов

Yungelson

2014

Living Rev. Relativ.

453

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.

453

382

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“…Yungelson, 1973, 1993;Massevitch et al, 1976), the position of the spiral arms will change considerably with respect to the stars and their tangent directions appear displaced with respect to the maxima of the HMXB population. The inner part of the Norma arm was at the position of the observed HMXB peak density approximately ∼15-20 million years ago which is in agreement with the model of Shtykovskiy and Gilfanov (2007).…”

Section: From Soriamentioning

confidence: 99%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

230

234

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High-mass X-ray binaries are fundamental in the study of stellar evolution, nucleosynthesis, structure and evolution of galaxies and accretion processes. Hard X-rays observations by INTEGRAL and Swift have broadened significantly our understanding in particular for the super-giant systems in the Milky Way, which number has increased by almost a factor of three. INTEGRAL played a crucial role in the discovery, study and understanding of heavily obscured systems and of fast X-ray transients. Most super-giant systems can now be classified in three categories: classical/obscured, eccentric and fast transient.The classical systems feature low eccentricity and variability factor of ∼ 10 3 , mostly driven by hydrodynamic phenomena occurring on scales larger than the accretion radius. Among them, systems with short orbital periods and close to Roche-Lobe overflow or with slow winds, appear highly obscured. In eccentric systems, the variability amplitude can reach even higher factors, because of the contrast of the wind density along the orbit. Four super-giant systems, featuring fast outbursts, very short orbital periods and anomalously low accretion rates, are not yet understood.Simulations of the accretion processes on relatively large scales have progressed and reproduce parts of the observations. The combined effects of wind

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“…A massive X-ray binary is an inevitable stage preceding the formation of a double compact system after the second supernova explosion of the helium-rich companion in such a stellar system. The formation scenario for binary pulsars proposed immediately after the discovery of PSR 1913+16 [106, 253] has also been tested by subsequent observations of binary pulsars. In fact, the scenario for binary pulsars was proposed even earlier in [415], but because no binary pulsars were known at that time, it was suggested that all pairs of NS are disrupted at the second NS formation.…”

Section: Evolutionary Scenario For Compact Binaries With Neutron Starmentioning

confidence: 99%

The Evolution of Compact Binary Star Systems

Постнов¹,

Yungelson

2006

Living Rev. Relativ.

119

114

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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). Binary NSs and BHs are thought to be the primary astrophysical sources of gravitational waves (GWs) within the frequency band of ground-based detectors, while compact binaries of WDs are important sources of GWs at lower frequencies to be covered by space interferometers (LISA). Major uncertainties in the current understanding of properties of NSs and BHs most relevant to the GW studies are discussed, including the treatment of the natal kicks which compact stellar remnants acquire during the core collapse of massive stars and the common envelope phase of binary evolution. We discuss the coalescence rates of binary NSs and BHs and prospects for their detections, the formation and evolution of binary WDs and their observational manifestations. Special attention is given to AM CVn-stars — compact binaries in which the Roche lobe is filled by another WD or a low-mass partially degenerate helium-star, as these stars are thought to be the best LISA verification binary GW sources.

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Evolution of massive close binaries and formation of neutron stars and black holes

Cited by 53 publications

References 12 publications

The Evolution of Compact Binary Star Systems

The Evolution of Compact Binary Star Systems

High-mass X-ray binaries in the Milky Way

The Evolution of Compact Binary Star Systems

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