COMPACT REMNANT MASS FUNCTION: DEPENDENCE ON THE EXPLOSION MECHANISM AND METALLICITY

By Chris L. Fryer, Krzysztof Belczyński, G. Wiktorowicz, M. Dominik, Vicky Kalogera, D. Holz. 2011

518 citations recorded by the source corpus.

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 supernova engines, we derive mass distributions of stellar compact remnants. We provide analytic prescriptions for both single-star models (as a function of initial star mass) and for binary-star models—prescriptions for compact object masses for major population synthesis codes. These prescriptions have implications for a range of observations: X-ray binary populations, supernova explosion energies, and gravitational wave sources. We show that advanced gravitational radiation detectors (like LIGO/VIRGO or the Einstein Telescope) will be able to further test the supernova explosion engine models once double black hole inspirals are detected.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/608c44091b4663416b17a14ed912a688df95344f

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Citations in the corpus

A simple approach to the supernova progenitor–explosion connection (2016, methodology): “Replacing the simple analytic arguments of Fryer (1999), Fryer & Kalogera (2001), Heger et al. (2003), Fryer et al. (2012), Belczynski et al. (2012), and Pejcha & Thompson (2015) with numerical calculations has an obvious downside, however, since this approach abandons the attractive, though very…”
Solving puzzles of GW150914 by primordial black holes (2016, background): “The scenario proposed in [11] is found to be the most appropriate.”
NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, methodology): “In the 25M stellar models discussed here, most or all of the s-process-rich material falls back forming a BH (the star in this case ends as a failed SN, see e.g., Woosley et al. 2002, and references therein), according to Fryer et al. (2012).”
The cosmic merger rate of stellar black hole binaries from the Illustris simulation (2017, methodology): “See also equation 1 and the text for details. where vBH is the natal kick for the BH, vNS is the natal kick for a NS (drawn from the distribution proposed by Hobbs et al. 2005), and ffb (ranging from 0 to 1) is the amount of fallback on the proto-NS (Fryer et al. 2012; Spera et al. 2015).”
DOUBLE COMPACT OBJECTS. II. COSMOLOGICAL MERGER RATES (2013, methodology): “This model also utilizes the “Rapid” convection-driven, neutrino-enhanced SN engine (Fryer et al. 2012).”
The cosmic merger rate of neutron stars and black holes (2018, background): “…of kick is scaled by the fallback as vBH = vNS (1− ffb), where vBH is the natal kick for the BH, vNS is the natal kick for a NS (drawn from a Maxwellian distribution as described above), and ffb (ranging from 0 to 1) is the amount of fallback on the proto-NS (Fryer et al. 2012; Spera et al. 2015).”
Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo (2018, background): “Moreover, only a subset of theoretical models (e.g., the “rapid” model in Fryer et al. 2012) reproduce this gap in stellar modeling.”
Massive runaway and walkaway stars (2018, methodology): “This assumption is equivalent to assuming a “BH velocity kick” (e.g., Belczynski et al. 2008; Fryer et al. 2012): BHs and NSs receive the same kick amplitude at birth, despite the differences in their masses.”
PROGENITOR-EXPLOSION CONNECTION AND REMNANT BIRTH MASSES FOR NEUTRINO-DRIVEN SUPERNOVAE OF IRON-CORE PROGENITORS (2012, background): “…masses leading to BH formation (e.g., Zhang et al. 2008; O’Connor & Ott 2011), and they raise doubts about claims in the literature that the possible gap between NS and BH masses requires explosions that set in relatively early after core bounce (Belczynski et al. 2011; Fryer et al. 2012).”
The effect of pair-instability mass loss on black-hole mergers (2016, methodology): “The final prescriptions for compact object mass are based on the mass of a star at the time of core collapse and the final mass of its carbon-oxygen core (Fryer et al. 2012).”
Constraining Formation Models of Binary Black Holes with Gravitational-wave Observations (2017, background): “These include mass-loss prescriptions for O and B stars known as the “Vink prescription” (Vink et al. 2001), metallicity dependence to the evolution of Wolf-Rayet stars (Vink & de Koter 2005), and prescriptions for the supernova mechanism developed in Fryer et al. (2012).”
Rapid and Bright Stellar-mass Binary Black Hole Mergers in Active Galactic Nuclei (2016, background): “To estimate the fraction of black holes that will reside in binaries with other black holes, we neglect natal kicks as most black holes are either born through direct collapse without a supernova explosion, or receive small natal kicks that will not disrupt the binary (Fryer et al. 2012).”
ASTROPHYSICAL IMPLICATIONS OF THE BINARY BLACK HOLE MERGER GW150914 (2016, background): “Fryer et al. (2012) find that the transition from NS to BH formation occurs at initial progenitor masses of ;18–20 M and the transition from fallback to complete BH collapse takes place at initial progenitor masses of ;40 M .”