The case for Case C mass transfer in the galactic evolution of black hole binaries

Brown, G. E.; Lee, Chang-Hwan

doi:10.1016/j.newast.2003.10.005

Cited by 5 publications

(6 citation statements)

References 16 publications

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“…It is uncertain how luminous a SN should be expected to be associated with the formation of a black hole by fallback, although expectations and observations tend to favour faint fallback SNe (see, e.g., Moriya et al 2010b). Despite this, support for strong shocks from fallback SNe would follow if SN 1987A were demonstrated to have formed a low-mass BH, as has occasionally been argued (Brown & Bethe 1994;Brown & Lee 2004).…”

Section: The Fate Of the Core: Black-hole Versusmentioning

confidence: 99%

Luminous Blue Variables and Superluminous Supernovae From Binary Mergers

Justham

Podsiadlowski

Vink

2014

ApJ

133

142

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Evidence suggests that the direct progenitor stars of some core-collapse supernovae (CCSNe) are luminous blue variables (LBVs), perhaps including some 'superluminous supernovae' (SLSNe). We examine models in which massive stars gain mass soon after the end of core hydrogen burning. These are mainly intended to represent mergers following a brief contact phase during early Case B mass transfer, but may also represent stars which gain mass in the Hertzsprung Gap or extremely late during the main-sequence phase for other reasons. The post-accretion stars spend their core helium-burning phase as blue supergiants (BSGs), and many examples are consistent with being LBVs at the time of core collapse. Other examples are yellow supergiants at explosion. We also investigate whether such post-accretion stars may explode successfully after core collapse. The final core properties of post-accretion models are broadly similar to those of single stars with the same initial mass as the pre-merger primary star. More surprisingly, when early Case B accretion does affect the final core properties, the effect appears likely to favour a successful SN explosion, i.e., to make the core properties more like those of a lower-mass single star. However, the detailed structures of these cores sometimes display qualitative differences to any single-star model we have calculated. The rate of appropriate binary mergers may match the rate of SNe with immediate LBV progenitors; for moderately optimistic assumptions we estimate that the progenitor birthrate is ∼1% of the CCSN rate.

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Section: The Fate Of the Core: Black-hole Versusmentioning

confidence: 99%

Luminous Blue Variables and Superluminous Supernovae From Binary Mergers

Justham

Podsiadlowski

Vink

2014

ApJ

133

142

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“…Then the accretion‐induced formation of a black hole may occur (see e.g. Brown & Lee for more details).…”

Section: The Modelsmentioning

confidence: 99%

“…The effect of the NS mass increase in the accretion state is generally less important, unless a hypercritical accretion (especially inside common envelopes) is allowed. Then the accretion-induced formation of a black hole may occur (see, e. g., Brown & Lee (2004) for more details).…”

Section: Evolution Of Neutron Starsmentioning

confidence: 99%

Population synthesis for symbiotic X-ray binaries

Lü

Zhu

Постнов

et al. 2012

Monthly Notices of the Royal Astronomical Society

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Symbiotic X‐ray binaries (SyXBs) comprise a rare class of low‐mass X‐ray binaries. We study the Galactic SyXBs, which we consider as detached binaries composed of low‐mass giants and wind‐fed neutron star (NS) companions, by simulation of the interaction of a magnetized NS with its environment and utilizing a population synthesis code. We focus mainly on the parameters that influence the observational appearance of an SyXB: the donor wind velocity (vw) and the angular momentum distribution in the shell of matter settling on to an NS. We estimate the birthrate of SyXBs as ∼4.1 × 10−5 to ∼6.6 × 10−6 yr−1 and their number in the Galaxy as ∼100–1000. The assumed stellar wind velocity from cool giants is the input parameter that influences the model SyXB population most. Among known SyXBs or candidate systems, 4U 1954+31 and IGR J16358−4724 in which the NSs have very long spin periods may host quasi‐spherically accreting NSs. GX 1+4 has a peculiar long‐term spin behaviour and it may also be a quasi‐spherical wind‐accreting source. We cannot identify whether there are wind‐fed accretion discs in 4U 1700+24, Sct X‐1, IRXS J180431.1−273932 and 2XMM J174016.0−290337.

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“…Several authors have considered late time mass transfer during a late stage of core helium burning or after core helium exhaustion (so-called Case C mass transfer) as a possible route to obtaining GRB-like conditions. This late time mass transfer can enable the formation of a massive stellar core, even at high metallicity (Brown and Lee 2004). Alternatively, depending on the properties of the binary this mass transfer may result in the formation of a common envelope, which will unbind the envelope of the star at the cost of the orbital energy (and hence separation).…”

Section: Binary Star Scenariosmentioning

confidence: 99%

Gamma-Ray Burst Progenitors

Levan¹,

Crowther²,

Grijs³

et al. 2016

Gamma-Ray Bursts

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We review our current understanding of the progenitors of both long and short duration gamma-ray bursts (GRBs). Constraints can be derived from multiple directions, and we use three distinct strands; (i) direct observations of GRBs and their host galaxies, (ii) parameters derived from modelling, both via population synthesis and direct numerical simulation and (iii) our understanding of plausible analog progenitor systems observed in the local Universe. From these joint constraints, we describe the likely routes that can drive massive stars to the creation of long GRBs, and our best estimates of the scenarios that can create compact object binaries which will ultimately form short GRBs, as well as the associated rates of both long and short GRBs. We further discuss how different the progenitors may be in the case of black hole engine or millisecond-magnetar models for the production of GRBs, and how central engines may provide a unifying theme between many classes of extremely luminous transient, from luminous and super-luminous supernovae to long and short GRBs.

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The case for Case C mass transfer in the galactic evolution of black hole binaries

Cited by 5 publications

References 16 publications

Luminous Blue Variables and Superluminous Supernovae From Binary Mergers

Luminous Blue Variables and Superluminous Supernovae From Binary Mergers

Population synthesis for symbiotic X-ray binaries

Gamma-Ray Burst Progenitors

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