Estimates of black hole natal kick velocities from observations of low-mass X-ray binaries

Mandel, Ilya

doi:10.1093/mnras/stv2733

Cited by 157 publications

(132 citation statements)

References 21 publications

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“…Most have been used to make predictions for the merger rates of compact objects and the mass range for such mergers (e.g. Bogomazov, Lipunov & Tutukov 2007;Lipunov & Pruzhinskaya 2014;de Mink & Belczynski 2015;Kowalska-Leszczynska et al 2015;Mandel 2016;Mandel & de Mink 2016). With the detection of GW 150914 we now have a first observational datum to compare against such models; a situation analogous to the first detection of a supernova progenitor star (that of SN 1987A, now known to be a rare progenitor type) in preexplosion imaging which provided an immediate constraint on stellar models (Walborn et al 1987;Podsiadlowski 1992).…”

Section: +4mentioning

confidence: 99%

“…For black hole kicks we assume a momentum distribution and reduce the kick velocity by multiplying it by 1.4M⊙ and dividing by the black hole mass. We do this because of the growing evidence as discussed by Mandel (2016) that black-hole kicks are smaller than those of neutron stars. The full method of determining kicks and the fate of the binary when a SN occurs within it are described in Eldridge, Langer & Tout (2011).…”

Section: Predicting the Remnant Masses And Sn Kick Velocitiesmentioning

confidence: 99%

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bpass predictions for binary black hole mergers

Eldridge

Stanway

2016

Mon. Not. R. Astron. Soc.

275

225

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Using the Binary Population and Spectral Synthesis code BPASS, we have calculated the rates, timescales and mass distributions for binary black hole mergers as a function of metallicity. We consider these in the context of the recently reported 1st LIGO event detection. We find that the event has a very low probability of arising from a stellar population with initial metallicity mass fraction above Z = 0.010 (Z > ∼ 0.5 Z ⊙ ). Binary black hole merger events with the reported masses are most likely in populations below 0.008 (Z < ∼ 0.4 Z ⊙ ). Events of this kind can occur at all stellar population ages from 3 Myr up to the age of the universe, but constitute only 0.1 to 0.4 per cent of binary BH mergers between metallicities of Z = 0.001 to 0.008. However at metallicity Z = 10 −4 , 26 per cent of binary BH mergers would be expected to have the reported masses. At this metallicity the progenitor merger times can be close to ≈ 10Gyr and rotationallymixed stars evolving through quasi-homogeneous evolution, due to mass transfer in a binary, dominate the rate. The masses inferred for the black holes in the binary progenitor of GW 150914 are amongst the most massive expected at anything but the lowest metallicities in our models. We discuss the implications of our analysis for the electromagnetic follow-up of future LIGO event detections.

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Section: +4mentioning

confidence: 99%

Section: Predicting the Remnant Masses And Sn Kick Velocitiesmentioning

confidence: 99%

bpass predictions for binary black hole mergers

Eldridge

Stanway

2016

Mon. Not. R. Astron. Soc.

275

225

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“…This motivated the proposition based on theoretical calculations that by the gravitational pull from asymmetric mass ejecta, BHs can be accelerated to velocities comparable to those of NSs 35 . However, because of the unknown origin and several other uncertainties of the samples of sources, it has been argued that from only the existing observations of the spatial locations of low-mass X-ray binaries, it is not possible to confidently infer the existence of high BH NKs 36 . In the following are reviewed the observations of the three runaway low mass BH-XRBs for which the space velocities in three dimensions have been determined: GRO J1655-40, XTE 1118+480 and V404 Cyg.…”

Section: Runaway Black Hole X-ray Binariesmentioning

confidence: 99%

The formation of stellar black holes

Mirabel

2017

New Astronomy Reviews

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Abstract:It is believed that stellar black holes (BHs) can be formed in two different ways: Either a massive star collapses directly into a BH without a supernova (SN) explosion, or an explosion occurs in a proto-neutron star, but the energy is too low to completely unbind the stellar envelope, and a large fraction of it falls back onto the short-lived neutron star (NS), leading to the delayed formation of a BH. Theoretical models set progenitor masses for BH formation by implosion, namely, by complete or almost complete collapse, but observational evidences have been elusive. Here are reviewed the observational insights on BHs formed by implosion without large natal kicks from: (1) the kinematics in three dimensions of space of five Galactic BH X-ray binaries (BH-XRBs), (2) the diversity of optical and infrared observations of massive stars that collapse in the dark, with no luminous SN explosions, possibly leading to the formation of BHs, and (3) the sources of gravitational waves produced by mergers of stellar BHs so far detected with LIGO. Multiple indications of BH formation without ejection of a significant amount of matter and with no natal kicks obtained from these different areas of observational astrophysics, and the recent observational confirmation of the expected dependence of BH formation on metallicity and redshift, are qualitatively consistent with the high merger rates of binary black holes (BBHs) inferred from the first detections with LIGO.

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“…Although many channels have been explored for the formation of such systems, most proposals fall into two categories: the "field" channel, in which BBHs are formed from isolated stellar binaries, usually involving either a common-envelope phase (e.g., Voss & Tauris 2003;Dominik et al 2012Dominik et al , 2013Belczynski et al 2016) or chemically homogeneous evolution due to rapid stellar rotation (e.g., De Mink & Mandel 2016;Marchant et al 2016), or the "dynamical" channel, in which BBHs are created though three-body encounters in dense star clusters (e.g., Sigurdsson & Hernquist 1993;Portegies Zwart & Mcmillan 2000;Downing et al 2010Downing et al , 2011Ziosi et al 2014;Rodriguez et al 2015Rodriguez et al , 2016a. Unfortunately, the masses and merger rates predicted by these models often significantly overlap, making it difficult to discriminate between different formation channels for BBHs even with multiple detections.…”

Section: Introductionmentioning

confidence: 99%

Illuminating Black Hole Binary Formation Channels With Spins in Advanced Ligo

Rodriguez

Zevin

Pankow

et al. 2016

ApJL

342

332

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The recent detections of the binary black hole mergers GW150914 and GW151226 have inaugurated the field of gravitational-wave astronomy. For the two main formation channels that have been proposed for these sources, isolated binary evolution in galactic fields and dynamical formation in dense star clusters, the predicted masses and merger rates overlap significantly, complicating any astrophysical claims that rely on measured masses alone. Here, we examine the distribution of spin-orbit misalignments expected for binaries from the field and from dense star clusters. Under standard assumptions for black hole natal kicks, we find that black hole binaries similar to GW150914 could be formed with significant spin-orbit misalignment only through dynamical processes. In particular, these heavy-black hole binaries can only form with a significant spin-orbit anti-alignment in the dynamical channel. Our results suggest that future detections of merging black hole binaries with measurable spins will allow us to identify the main formation channel for these systems.

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Estimates of black hole natal kick velocities from observations of low-mass X-ray binaries

Cited by 157 publications

References 21 publications

bpass predictions for binary black hole mergers

bpass predictions for binary black hole mergers

The formation of stellar black holes

Illuminating Black Hole Binary Formation Channels With Spins in Advanced Ligo

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