Compact Remnant Mass Function: Dependence on the Explosion Mechanism and Metallicity

  title={Compact Remnant Mass Function: Dependence on the Explosion Mechanism and Metallicity},
  author={Christopher L. Fryer and Krzysztof Belczynski and Grzegorz Wiktorowicz and Michał Dominik and Vassiliki Kalogera and Daniel E. Holz},
  journal={The Astrophysical Journal},
The mass distribution of neutron stars and stellar-mass black holes provides vital clues into the nature of stellar core collapse and the physical engine responsible for supernova explosions. A number of supernova engines have been proposed: neutrino- or oscillation-driven explosions enhanced by early (developing in 10-50 ms) and late-time (developing in 200 ms) convection as well as magnetic field engines (in black hole accretion disks or neutron stars). Using our current understanding of… 
Confronting Models of Massive Star Evolution and Explosions with Remnant Mass Measurements
The mass distribution of compact objects provides a fossil record that can be studied to uncover information on the late stages of massive star evolution, the supernova explosion mechanism, and the
We perform hydrodynamic supernova (SN) simulations in spherical symmetry for over 100 single stars of solar metallicity to explore the progenitor-explosion and progenitor-remnant connections
The mass spectrum of compact remnants from the parsec stellar evolution tracks
The mass spectrum of stellar-mass black holes (BHs) is highly uncertain. Dynamical mass measurements are available only for few ( 10) BHs in X-ray binaries, while theoretical models strongly depend
Pre-supernova evolution, compact-object masses, and explosion properties of stripped binary stars
The era of large transient surveys, gravitational-wave observatories, and multi-messenger astronomy has opened up new possibilities for our understanding of the evolution and final fate of massive
The observed neutron star mass distribution as a probe of the supernova explosion mechanism
The observed distribution of neutron star (NS) masses reflects the physics of core-collapse supernova explosions and the structure of the massive stars that produce them at the end of their
Distinguishing compact binary population synthesis models using gravitational-wave observations of coalescing binary black holes
The coalescence of compact binaries containing neutron stars or black holes is one of the most promising signals for advanced ground-based laser interferometer gravitational-wave detectors, with the
Gas depletion in primordial globular clusters due to accretion on to stellar-mass black holes
We consider the effect of compact stellar remnants on the interstellar medium of a massive star cluster following the initial burst of star formation. We argue that accretion onto stellar-mass black
A simple approach to the supernova progenitor–explosion connection
We present a new approach to understand the landscape of supernova explosion energies, ejected nickel masses, and neutron star birth masses. In contrast to other recent parametric approaches, our
Black-Hole Remnants from Black-Hole-Neutron-Star Mergers.
It is predicted that black-hole-neutron-star mergers produce a population of remnant black holes with masses distributed around 7  M_{⊙} and 9‬‬M{�’}.
Rapid and Bright Stellar-mass Binary Black Hole Mergers in Active Galactic Nuclei
The Laser Interferometer Gravitational-Wave Observatory, LIGO, found direct evidence for double black hole binaries emitting gravitational waves. Galactic nuclei are expected to harbor the densest


Fallback and Black Hole Production in Massive Stars
The compact remnants of core-collapse supernovae?neutron stars and black holes?have properties that reflect both the structure of their stellar progenitors and the physics of the explosion. In
Formation Rates of Black Hole Accretion Disk Gamma-Ray Bursts
The cosmological origin of at least an appreciable fraction of classical gamma-ray bursts (GRBs) is now supported by redshift measurements for a half-dozen faint host galaxies. Still, the nature of
The evolution and explosion of massive stars
Like all true stars, massive stars are gravitationally confined thermonuclear reactors whose composition evolves as energy is lost to radiation and neutrinos. Unlike lower-mass stars (M≲8M⊙),
A Comprehensive Study of Binary Compact Objects as Gravitational Wave Sources: Evolutionary Channels, Rates, and Physical Properties
A new generation of ground-based interferometric detectors for gravitational waves is currently under construction or has entered the commissioning phase (Laser Interferometer Gravitational-wave
We present two-dimensional hydrodynamic simulations of stellar core collapse and develop the framework for a detailed analysis of the energetic aspects of neutrino-powered supernova explosions. Our
The Neutron star and black hole initial mass function
Using recently calculated models for massive stellar evolution and supernovae coupled to a model for Galactic chemical evolution, neutron star and black hole birth functions (number of neutron stars
A two-solar-mass neutron star measured using Shapiro delay
Radio timing observations of the binary millisecond pulsar J1614-2230 that show a strong Shapiro delay signature are presented and the pulsar mass is calculated to be (1.97 ± 0.04)M⊙, which rules out almost all currently proposed hyperon or boson condensate equations of state.
Collapsars: Gamma-ray bursts and explosions in 'failed supernovae'
Using a two-dimensional hydrodynamics code (PROMETHEUS), we explore the continued evolution of rotating helium stars, Mα 10 M☉, in which iron-core collapse does not produce a successful outgoing
Theoretical black hole mass distributions
We derive the theoretical distribution function of black hole masses by studying the formation processes of black holes. We use the results of recent two-dimensional simulations of stellar core
Multidimensional supernova simulations with approximative neutrino transport. I. Neutron star kicks and the anisotropy of neutrino-driven explosions in two spatial dimensions
We study hydrodynamic instabilities during the first seconds of core-collapse supernovae by means of 2D simulations with approximative neutrino transport and boundary conditions that parameterize the