The formation of stellar black holes

Mirabel, F.

doi:10.1016/j.newar.2017.04.002

Cited by 64 publications

(50 citation statements)

References 99 publications

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“…The current theoretical understanding does not show a direct correlation and suggests that there is no clean mass cut off for direct collapse formation (Sukhbold et al 2016). We have obtained observational constraints on the potential kicks of 16 BHXBs (Figure 10), which increases the sample size and updates the estimations of BHXB kicks by Mirabel (2017) and Gandhi et al (2019) (current peculiar velocity used as proxy in both works). We conducted correlation tests, which indicated negligible correlation between BH mass and kick, with a Pearson Rank coefficient of −0.23 ± 0.17 (p=0.21) and a Spearman Rank coefficient of −0.2 ± 0.17 (p=0.40).…”

Section: Natal Kicks and Black Hole Massmentioning

confidence: 86%

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Potential kick velocity distribution of black hole X-ray binaries and implications for natal kicks

Atri

Miller-Jones

Bahramian

et al. 2019

Monthly Notices of the Royal Astronomical Society

120

102

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We use Very Long Baseline Interferometry to measure the proper motions of three black hole X-ray binaries (BHXBs). Using these results together with data from the literature and Gaia-DR2 to collate the best available constraints on proper motion, parallax, distance and systemic radial velocity of 16 BHXBs, we determined their three dimensional Galactocentric orbits. We extended this analysis to estimate the probability distribution for the potential kick velocity (PKV) a BHXB system could have received on formation. Constraining the kicks imparted to BHXBs provides insight into the birth mechanism of black holes (BHs). Kicks also have a significant effect on BH-BH merger rates, merger sites, and binary evolution, and can be responsible for spin-orbit misalignment in BH binary systems. 75% of our systems have potential kicks > 70 km s −1 . This suggests that strong kicks and hence spin-orbit misalignment might be common among BHXBs, in agreement with the observed quasi-periodic X-ray variability in their power density spectra. We used a Bayesian hierarchical methodology to analyse the PKV distribution of the BHXB population, and suggest that a unimodal Gaussian model with a mean of 107±16 km s −1 is a statistically favourable fit. Such relatively high PKVs would also reduce the number of BHs likely to be retained in globular clusters. We found no significant correlation between the BH mass and PKV, suggesting a lack of correlation between BH mass and the BH birth mechanism. Our Python code allows the estimation of the PKV for any system with sufficient observational constraints.

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Section: Natal Kicks and Black Hole Massmentioning

confidence: 86%

“…Attempts have been made to understand if there is any relation between BH mass and the natal kick it receives (Mirabel 2017). This could assist in understanding the correlation between the final pathway a progenitor takes to become a BH and the mass of the BH.…”

Section: Natal Kicks and Black Hole Massmentioning

confidence: 99%

Potential kick velocity distribution of black hole X-ray binaries and implications for natal kicks

Atri

Miller-Jones

Bahramian

et al. 2019

Monthly Notices of the Royal Astronomical Society

120

102

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“…There are a few (indirect) observational tests for binary misalignment. For instance, the proper motion of Cygnus X-1 is consistent with that of its natal association of O stars, implying that it felt no supernova kick [145]. Before we get excited that this explains why Cygnus X-1 has no QPOs however, we must also note that GRS 1915+105, which has very strong QPOs, also has no peculiar velocity with respect to its association [145].…”

Section: Are These Systems Misaligned?mentioning

confidence: 92%

“…For instance, the proper motion of Cygnus X-1 is consistent with that of its natal association of O stars, implying that it felt no supernova kick [145]. Before we get excited that this explains why Cygnus X-1 has no QPOs however, we must also note that GRS 1915+105, which has very strong QPOs, also has no peculiar velocity with respect to its association [145]. Another test comes from super-luminal jet ejections, because the 3D jet trajectory can be reconstructed by tracking the proper motion and brightness of approaching and receding lobes.…”

Section: Are These Systems Misaligned?mentioning

confidence: 92%

A review of quasi-periodic oscillations from black hole X-ray binaries: Observation and theory

Ingram

Motta

2019

New Astronomy Reviews

253

176

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Black hole and neutron star X-ray binary systems routinely show quasiperiodic oscillations (QPOs) in their X-ray flux. Despite being strong, easily measurable signals, their physical origin has long remained elusive. However, recent observational and theoretical work has greatly improved our understanding. Here, we briefly review the basic phenomenology of the different varieties of QPO in both black hole and neutron star systems before focusing mainly on low frequency QPOs in black hole systems, for which much of the recent progress has been made. We describe the detailed statistical properties of these QPOs and review the physical models proposed in the literature, with particular attention to those based on Lense-Thirring precession. This is a relativistic effect whereby a spinning massive object twists up the surrounding spacetime, inducing nodal precession in inclined orbits. We review the theory describing how an accretion flow reacts to the Lense-Thirring effect, including analytic theory and recent numerical simulations. We then describe recent observational tests that provide very strong evidence that at least a certain type of low frequency QPOs are a geometric effect, and good evidence that they are the result of precession. We discuss the possibility of the spin axis of the compact object being misaligned with the binary rotation axis for a large fraction of X-ray binaries, as is required for QPOs to be driven specifically by Lense-Thirring precession, as well as some outstanding gaps in our understanding and future opportunities provided by X-ray polarimeters and/or high throughput X-ray detectors.

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“…Kalogera 1999;Podsiadlowski, Rappaport & Han 2003;Kiel & Hurley 2006). Meanwhile, the observed scale height is driven by the presence of natal kicks, a current hot topic in the field (Jonker & Nelemans 2004;Fragos et al 2009;Repetto et al 2017;Mirabel 2017;Casares, Jonker & Israelian 2017). It should be stressed here that, even if the total number of discovered BHs turns out to be lower than predicted, HAWKs will still set stringent constraints on BH formation models.…”

Section: Discussionmentioning

confidence: 99%

Hibernating black holes revealed by photometric mass functions

Casares

2017

Monthly Notices of the Royal Astronomical Society

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We present a novel strategy to uncover the Galactic population of quiescent black holes (BHs). This is based on a new concept , the photometric mass function (PMF), which opens up the possibility of an efficient identification of dynamical BHs in large fields-of-view. This exploits the width of the disc Hα emission line, combined with orbital period information. We here show that Hα widths can be recovered using a combination of customized Hα filters. By setting a width cut-off at 2200 km s −1 we are able to cleanly remove other Galactic populations of Hα emitters, including ∼99.9% of cataclysmic variables (CVs). Only short period (P orb <2.1 h) eclipsing CVs and AGNs will contaminate the sample but these can be easily flagged through photometric variability and, in the latter case, also mid-IR colours. We also describe the strategy of a deep (r=22) Galactic plane survey based on the concept of PMFs: HAWKs, the HAlpha-Width Kilo-deg Survey. We estimate that ∼800 deg 2 are required to unveil ∼50 new dynamical BHs, a three-fold improvement over the known population. For comparison, a century would be needed to produce an enlarged sample of 50 dynamical BHs from X-ray transients at the current discovery rate.

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The formation of stellar black holes

Cited by 64 publications

References 99 publications

Potential kick velocity distribution of black hole X-ray binaries and implications for natal kicks

Potential kick velocity distribution of black hole X-ray binaries and implications for natal kicks

A review of quasi-periodic oscillations from black hole X-ray binaries: Observation and theory

Hibernating black holes revealed by photometric mass functions

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