SPH Simulations of the Induced Gravitational Collapse Scenario of Long Gamma-Ray Bursts Associated with Supernovae

Becerra, L.; Ellinger, C. L.; Fryer, C. L.; Rueda, J. A.; Ruffini, R.

doi:10.3847/1538-4357/aaf6b3

Title: SPH Simulations of the Induced Gravitational Collapse Scenario of Long Gamma-Ray Bursts Associated with Supernovae

Journal Article · Fri Jan 18 00:00:00 EST 2019 · The Astrophysical Journal (Online)

DOI:https://doi.org/10.3847/1538-4357/aaf6b3· OSTI ID:1524403

Becerra, L. ^[1]; Ellinger, C. L. ^[2];

^[2];

^[3]; Ruffini, R. ^[3]

Sapienza Univ. di Roma, Rome (Italy); ICRANet, Pescara (Italy)
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Sapienza Univ. di Roma, Rome (Italy); ICRANet, Pescara (Italy); ICRANet-Rio, Rio de Janeiro (Brazil)

We present the first three-dimensional smoothed particle hydrodynamics simulations of the induced gravitational collapse scenario of long-duration gamma-ray bursts (GRBs) associated with supernovae (SNe). We simulate the SN explosion of a carbon–oxygen core (CO_core) forming a binary system with a neutron star (NS) companion. We follow the evolution of the SN ejecta, including their morphological structure, subject to the gravitational field of both the new NS (νNS) formed at the center of the SN and the one of the NS companion. We compute the accretion rate of the SN ejecta onto the NS companion, as well as onto the νNS from SN matter fallback. We determine the fate of the binary system for a wide parameter space including different CO_core and NS companion masses, orbital periods, and SN explosion geometry and energies. We identify, for selected NS nuclear equations of state, the binary parameters leading the NS companion, by hypercritical accretion, either to the mass-shedding limit or to the secular axisymmetric instability for gravitational collapse to a black hole (BH), or to a more massive, fast-rotating, stable NS. We also assess whether the binary remains gravitationally bound after the SN explosion, hence exploring the space of binary and SN explosion parameters leading to νNS–NS and νNS–BH binaries. As a result, the consequences of our results for the modeling of long GRBs, i.e., X-ray flashes and binary-driven hypernovae, are discussed.

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Research Organization:: Los Alamos National Lab. (LANL), Los Alamos, NM (United States)

Sponsoring Organization:: USDOE National Nuclear Security Administration (NNSA), Office of Defense Nuclear Nonproliferation

Grant/Contract Number:: 89233218CNA000001

OSTI ID:: 1524403

Report Number(s):: LA-UR-18-21187

Journal Information:: The Astrophysical Journal (Online), Vol. 871, Issue 1; ISSN 1538-4357

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 29 works

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Mass Limits For Black Hole Formation Fryer, C. L. arXiv https://doi.org/10.48550/arxiv.astro-ph/9902315	text	January 1999

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Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
Astronomy and Astrophysics
accretion
accretion disks
binaries: close
gamma-ray burst: general
supernovae: general
stars: black holes
stars: neutron

Title: SPH Simulations of the Induced Gravitational Collapse Scenario of Long Gamma-Ray Bursts Associated with Supernovae

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