Formation Channels of Single and Binary Stellar-Mass Black Holes

Mapelli, Michela

doi:10.1007/978-981-15-4702-7_16-1

Cited by 47 publications

(35 citation statements)

References 344 publications

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“…Where initially stated in different units, we convert these, using, as appropriate, factors of 1:7 Â 10 10 solar blue-light luminosities per Milky Way equivalent galaxy (MWEG), 1:17 Â 10 À2 MWEG per Mpc 3 (Kopparapu et al 2008), a globular cluster space density of 2.9 per Mpc 3 at z ¼ 0 (Portegies Zwart and McMillan 2000) and a local supernova rate of 1:06 Â 10 5 Gpc À3 yr À1 (Taylor et al 2014). Of course, such simple re-scalings do not account for the dependence of merger rates on the star formation history and metallicity (de Freitas Pacheco et al 2006;Belczynski et al 2010;Dvorkin et al 2016;Neijssel et al 2019;Mapelli 2021).…”

Section: Executive Summarymentioning

confidence: 99%

Rates of compact object coalescences

2022

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Gravitational-wave detections are enabling measurements of the rate of coalescences of binaries composed of two compact objects—neutron stars and/or black holes. The coalescence rate of binaries containing neutron stars is further constrained by electromagnetic observations, including Galactic radio binary pulsars and short gamma-ray bursts. Meanwhile, increasingly sophisticated models of compact objects merging through a variety of evolutionary channels produce a range of theoretically predicted rates. Rapid improvements in instrument sensitivity, along with plans for new and improved surveys, make this an opportune time to summarise the existing observational and theoretical knowledge of compact-binary coalescence rates.

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Section: Executive Summarymentioning

confidence: 99%

Rates of compact object coalescences

2022

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“…The inferred distribution can be used to compute constraints on BBH formation channel models, most broadly divided into dynamical formation in dense environments [20][21][22][23], such as star clusters [24][25][26][27][28] and active galactic nuclei (AGN) disks [29][30][31][32][33][34]); and binary co-evolution in isolation [35][36][37][38][39][40][41][42] or with external agents [43][44][45][46][47][48][49]. Refer to Mapelli [50] for a recent review of formation channels.…”

Section: Introductionmentioning

confidence: 99%

New binary black hole mergers in the LIGO--Virgo O3a data

Olsen¹,

Venumadhav²,

Mushkin³

et al. 2022

Preprint

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We report the detection of ten new binary black hole (BBH) merger signals in the publicly released data from the the first half of the third observing run (O3a) of advanced LIGO and advanced Virgo. Candidates are identified using an updated version of the search pipeline described in Venumadhav et al.[1] (the "IAS pipeline" [2]), and events are declared according to criteria similar to those in the GWTC-2.1 catalog [3]. The updated search is sensitive to a larger region of parameter space, applies a template prior that accounts for different search volume as a function of intrinsic parameters, and uses an improved coherent detection statistic that optimally combines the data from the Hanford and Livingston detectors. Among the ten new events, we observe interesting astrophysical scenarios including sources with confidently large effective spin parameters in both the positive and negative directions, high-mass black holes that are difficult to form in stellar collapse models due to (pulsational) pair instability, and low-mass mergers that bridge the gap between neutron stars and the lightest observed black holes. We detect events populating the upper and lower black hole mass gaps with both extreme and near-unity mass ratios, and one of the possible neutron star-black hole (NSBH) mergers is well localized for electromagnetic (EM) counterpart searches. We see a substantial increase in significance for many of the events previously reported by other pipelines, and we detect all of the GWTC-2.1 BBH mergers with coincident data in Hanford and Livingston except for three loud events that get vetoed, which is compatible with the falsepositive rate of our veto procedure, and three that fall below the detection threshold. We also return to significance the event GW190909 114149, which was reduced to a sub-threshold trigger after its initial appearance in . This amounts to a total of 42 BBH mergers detected by our pipeline's search of the coincident Hanford-Livingston O3a data.

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“…The astrophysical interpretation of GW detections is crucial to shed light on the evolutionary history of compact-object binaries. We still do not know how heavy stellar black holes form, how two black holes can merge within a Hubble time, and what are the distinguishing features that would allow us to piece-together the formation pathways of compact-object binaries [14,15].…”

Section: Introductionmentioning

confidence: 99%

“…At the same time, the orbital period of tight binaries can be as short as ∼days [46,47]. Furthermore, it is also crucial to consider time-scales related to binary stellar evolution, such as the typical timescale for stable mass transfer (SMT) O 10 3 yr, or the common envelope (CE) time scale, that is O 10 3 − 10 5 yr [15]. N-body simulations that aim at investigating merging compact objects in GCs need to cover, at least, t relax (∼Gyrs) of evolution and to resolve all the mentioned timescales simultaneously.…”

Section: Introductionmentioning

confidence: 99%

ISTEDDAS: a new direct N-Body code to study merging compact-object binaries

Mencagli

Nazarova

Spera

2022

J. Phys.: Conf. Ser.

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On September 14, 2015, the two detectors of the Laser Interferometer Gravitational wave Observatory (LIGO) reported the first detection of gravitational waves, a signal generated from the coalescence of two stellar-mass black holes. The discovery represented the beginning of an entirely new way to investigate the Universe. From the theoretical point of view, the formation and evolution of compact-object binaries are still very uncertain. One of the main issues is that most stars form in dense stellar environments, and numerical simulations of merging compact-object binaries in such crowded stellar systems are very challenging. In this work, we review the main numerical bottlenecks that hamper our knowledge on merging binaries in dense environments and we present a new GPU-accelerated N-body code, which is currently under development, called isteddas, that can overcome most of the obstacles.

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Formation Channels of Single and Binary Stellar-Mass Black Holes

Cited by 47 publications

References 344 publications

Rates of compact object coalescences

Rates of compact object coalescences

New binary black hole mergers in the LIGO--Virgo O3a data

ISTEDDAS: a new direct N-Body code to study merging compact-object binaries

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