On the Mechanism of Accretion by Stars

Bondi, Hermann; Hoyle, F.

doi:10.1093/mnras/104.5.273

Cited by 1,547 publications

(1,285 citation statements)

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“…Current estimates indicate that there are between 0.1-1 billion such systems within our Galaxy, a very small fraction of which, < 0.001%, might be detectable in a deep X-ray survey of the Galactic plane [31]. Even a so-called isolated black hole will accrete at some level from the surrounding gaseous interstellar medium (ISM) -this mode of accretion is called Bondi-Hoyle accretion after Herman Bondi and Fred Hoyle who calculated the details of this process [32]. Low-level X-ray emission is expected due to Bondi-Hoyle accretion, although there are large uncertainties regarding both the mass flux and radiative efficiency of the accretion flow [31].…”

Section: Stellar Mass Black Hole Systems and X-ray Binariesmentioning

confidence: 99%

Fluorescent iron lines as a probe of astrophysical black hole systems

2003

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Section: Stellar Mass Black Hole Systems and X-ray Binariesmentioning

confidence: 99%

Fluorescent iron lines as a probe of astrophysical black hole systems

2003

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“…The Bondi-Hoyle-Lyttleton (BHL, Bondi & Hoyle 1944;Hoyle & Lyttleton 1939) accretion radius can be a considerable fraction of the stellar radius. The accretion rate estimated by Brown (1995) and Chevalier (1996), when including highly-efficient neutrino cooling, is large enough to favour the formation of BH-NS systems over NS-NS systems.…”

Section: Introductionmentioning

confidence: 99%

Dynamics of jets during the common-envelope phase

Méndez

López-Cámara

Colle

2017

Monthly Notices of the Royal Astronomical Society

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Common envelope (CE) is an important phase in the evolution of many binary systems. Giant star / compact object interaction in binaries plays an important role in highenergy phenomena as well as in the evolution of their environment. Material accreted onto the compact object may form a disk and power a jet. We study analytically and through numerical simulations the interaction between the jet and the CE. We determine the conditions under which accreting material quenches the jet or allows it to propagate successfully, in which case even the envelope may be ejected. Close to the stellar core of the companion the compact object accretes at a larger rate. A jet launched from this region needs a larger accretion-to-ejection efficiency to successfully propagate through the CE compared to a jet launched far from the stellar core, and is strongly deflected by the orbital motion. The energy deposited by the jet may be larger than the binding energy of the envelope. The jet can, thus, play a fundamental role in the CE evolution. We find that the energy dissipation of the jet into the CE may stop accretion onto the disk. We expect the jet to be intermittent, unless the energy deposited is large enough to lead to the unbinding of the outer layers of the CE. Given that the energy and duration of the jet are similar to those of ultra-long GRBs, we suggest this as a new channel to produce these events.

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“…One of the SBHs began at the center of the circumnuclear disk, while the second SBH spiraled inwards from an initial separation of 50 pc to a final separation of ∼ 10 pc. Gas particles within the Bondi-Hoyle radii [18] of the SBHs were accreted, and assumed to fuel warped accretion disks as described in Perego et al [15]. On a timescale of 1-2 Myr, the SBH spins became aligned to within 10 • (30 • ) of their orbital angular momentum for a cold (hot) circumnuclear disk [19].…”

Section: Introductionmentioning

confidence: 99%

Effects of post-Newtonian spin alignment on the distribution of black-hole recoils

2012

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Recent numerical relativity simulations have shown that the final black hole produced in a binary merger can recoil with a velocity as large as 5, 000 km/s. Because of enhanced gravitational-wave emission in the so-called "hang-up" configurations, this maximum recoil occurs when the black-hole spins are partially aligned with the orbital angular momentum. We revisit our previous statistical analysis of post-Newtonian evolutions of black-hole binaries in the light of these new findings. We demonstrate that despite these new configurations with enhanced recoil velocities, spin alignment during the post-Newtonian stage of the inspiral will still significantly suppress (or enhance) kick magnitudes when the initial spin of the more massive black hole is more (or less) closely aligned with the orbital angular momentum than that of the smaller hole. We present a preliminary study of how this post-Newtonian spin alignment affects the ejection probabilities of supermassive black holes from their host galaxies with astrophysically motivated mass ratio and initial spin distributions. We find that spin alignment suppresses (enhances) ejection probabilities by ∼ 40% (20%) for an observationally motivated mass-dependent galactic escape velocity, and by an even greater amount for a constant escape velocity of 1,000 km/s. Kick suppression is thus at least a factor two more efficient than enhancement.

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On the Mechanism of Accretion by Stars

Cited by 1,547 publications

References 0 publications

Fluorescent iron lines as a probe of astrophysical black hole systems

Fluorescent iron lines as a probe of astrophysical black hole systems

Dynamics of jets during the common-envelope phase

Effects of post-Newtonian spin alignment on the distribution of black-hole recoils

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