The spin of the second-born black hole in coalescing binary black holes

  title={The spin of the second-born black hole in coalescing binary black holes},
  author={Y. P. Qin and Tassos Fragos and Georges Meynet and Jeff J. Andrews and Mads S{\o}rensen and H. Francis Song},
  journal={Astronomy \& Astrophysics},
Context. Various binary black hole formation channels have been proposed since the first gravitational event GW150914 was discovered by the Advanced Laser Interferometer Gravitational-Wave Observatory (AdLIGO). The immediate progenitor of the binary black hole is a close binary system composed of a black hole and a helium star, which can be the outcome of the classical isolated binary evolution through the common envelope, or alternatively of the massive close evolution through chemically… 
The origin of spin in binary black holes
Context. After years of scientific progress, the origin of stellar binary black holes is still a great mystery. Several formation channels for merging black holes have been proposed in the
Coalescence of Kerr Black Holes—Binary Systems from GW150914 to GW170814
This work investigates the energy of the gravitational wave from a binary black hole merger by the coalescence of two Kerr black holes with an orbital angular momentum and ensures that the final black hole obtains a large portion of its spin angular momentum from the orbital orbital momentum of the initialbinary black hole.
Black Hole Formation in Fallback Supernova and the Spins of LIGO Sources
Here we investigate within the context of field binary progenitors how the the spin of the Laser Interferometer Gravitational Wave Observatory (LIGO) sources vary when the helium star-descendant
Spin Evolution of Stellar-mass Black Hole Binaries in Active Galactic Nuclei
The astrophysical origin of gravitational-wave (GW) events is one of the most timely problems in the wake of the LIGO/Virgo discoveries. In active galactic nuclei (AGNs), binaries form and evolve
An Alternative Interpretation of GW190412 as a Binary Black Hole Merger with a Rapidly Spinning Secondary
The Laser Interferometer Gravitational-Wave Observatory (LIGO)-Virgo collaboration recently reported the properties of GW190412, a binary black hole merger with unequal component masses (mass ratio
Formation Channels of Single and Binary Stellar-Mass Black Holes
  • M. Mapelli
  • Physics
    Handbook of Gravitational Wave Astronomy
  • 2021
These are exciting times for binary black hole (BBH) research. LIGO and Virgo detections are progressively drawing a spectacular fresco of BBH masses, spins and merger rates. In this review, we
The impact of mass-transfer physics on the observable properties of field binary black hole populations
We study the impact of mass-transfer physics on the observable properties of binary black hole populations that formed through isolated binary evolution. We used the POSYDON framework to combine
Black Hole Genealogy: Identifying Hierarchical Mergers with Gravitational Waves
In dense stellar environments, the merger products of binary black hole mergers may undergo additional mergers. These hierarchical mergers are naturally expected to have higher masses than the first
Pathways for producing binary black holes with large misaligned spins in the isolated formation channel
Binary black holes (BBHs) can form from the collapsed cores of isolated high-mass binary stars. The masses and spins of these BBHs are determined by the complicated interplay of phenomena such as
Fingerprints of Binary Black Hole Formation Channels Encoded in the Mass and Spin of Merger Remnants
Binary black holes (BBHs) are thought to form in different environments, including the galactic field and (globular, nuclear, young, and open) star clusters. Here, we propose a method to estimate the


Formation of close binary black holes merging due to gravitational-wave radiation
The conditions for the formation of close-binary black-hole systems merging over the Hubble time due to gravitational-wave radiation are considered in the framework of current ideas about the
The first gravitational-wave source from the isolated evolution of two stars in the 40–100 solar mass range
High-precision numerical simulations of the formation of binary black holes via the evolution of isolated binary stars are reported, providing a framework within which to interpret the first gravitational-wave source, GW150914, and to predict the properties of subsequent binary-black-hole gravitational- wave events.
A new route towards merging massive black holes
Recent advances in gravitational-wave astronomy make the direct detection of gravitational waves from the merger of two stellar-mass compact objects a realistic prospect. Evolutionary scenarios
Galactic field black hole (BH) low-mass X-ray binaries (LMXBs) are believed to form in situ via the evolution of isolated binaries. In the standard formation channel, these systems survived a common
Distinguishing spin-aligned and isotropic black hole populations with gravitational waves
The best-measured combination of spin parameters for each of the four likely binary black hole detections GW150914, LVT151012, GW151226 and GW170104 is the ‘effective’ spin, indicating that the effective spins for these systems indicate a 0.015 odds ratio against an aligned angular distribution compared to an isotropic one.
We explore the possibility that GW150914, the binary black hole (BBH) merger recently detected by Advanced LIGO, was formed by gravitational interactions in the core of a dense star cluster. Using
Implications of the Low Binary Black Hole Aligned Spins Observed by LIGO
We explore the implications of the low-spin components along the orbital axis observed in an Advanced LIGO O1 run on binary black hole (BBH) merger scenarios in which the merging BBHs have evolved
Astrophysical Implications of the Binary Black-Hole Merger GW150914
The discovery of the gravitational-wave (GW) source GW150914 with the Advanced LIGO detectors provides the first observational evidence for the existence of binary black hole (BH) systems that
Mass Limits For Black Hole Formation
We present a series of two-dimensional core-collapse supernova simulations for a range of progenitor masses and different input physics. These models predict a range of supernova energies and compact
Research Note: The Expected Spins of Gravitational Wave Sources With Isolated Field Binary Progenitors
We explore the consequences of dynamical evolution of field binaries composed of a primary black hole (BH) and a Wolf-Rayet (WR) star in the context of gravitational wave (GW) source progenitors. We