Angular momentum role in the hypercritical accretion of binary-driven hypernovae
Abstract
Here, the induced gravitational collapse paradigm explains a class of energetic, $${E}_{{\rm{iso}}}\gtrsim {10}^{52}$$ erg, long-duration gamma-ray bursts (GRBs) associated with Ic supernovae, recently named binary-driven hypernovae. The progenitor is a tight binary system formed of a carbon–oxygen (CO) core and a neutron star (NS) companion. The supernova ejecta of the exploding CO core trigger a hypercritical accretion process onto the NS, which reaches the critical mass in a few seconds, and gravitationally collapses to a black hole, emitting a GRB. In our previous simulations of this process, we adopted a spherically symmetric approximation to compute the features of the hypercritical accretion process. We here present the first estimates of the angular momentum transported by the supernova ejecta, $${L}_{{\rm{acc}}},$$ and perform numerical simulations of the angular momentum transfer to the NS during the hyperaccretion process in full general relativity. We show that the NS (1) reaches either the mass-shedding limit or the secular axisymmetric instability in a few seconds depending on its initial mass, (2) reaches a maximum dimensionless angular momentum value, $${[{cJ}/({{GM}}^{2})]}_{{\rm{max}}}\approx 0.7$$, and (3) can support less angular momentum than the one transported by supernova ejecta, $${L}_{{\rm{acc}}}\gt {J}_{{\rm{NS,max}}},$$ hence there is an angular momentum excess that necessarily leads to jetted emission.
- Authors:
-
- 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)
- Publication Date:
- Research Org.:
- Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)
- Sponsoring Org.:
- USDOE
- OSTI Identifier:
- 1329681
- Report Number(s):
- LA-UR-15-23118
Journal ID: ISSN 1538-4357
- Grant/Contract Number:
- AC52-06NA25396
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal (Online)
- Additional Journal Information:
- Journal Name: The Astrophysical Journal (Online); Journal Volume: 812; Journal Issue: 2; Journal ID: ISSN 1538-4357
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; astronomy and astrophysics; gamma-ray burst: general
Citation Formats
Becerra, L., Cipolletta, F., Fryer, Chris L., Rueda, Jorge A., and Ruffini, Remo. Angular momentum role in the hypercritical accretion of binary-driven hypernovae. United States: N. p., 2015.
Web. doi:10.1088/0004-637X/812/2/100.
Becerra, L., Cipolletta, F., Fryer, Chris L., Rueda, Jorge A., & Ruffini, Remo. Angular momentum role in the hypercritical accretion of binary-driven hypernovae. United States. https://doi.org/10.1088/0004-637X/812/2/100
Becerra, L., Cipolletta, F., Fryer, Chris L., Rueda, Jorge A., and Ruffini, Remo. Mon .
"Angular momentum role in the hypercritical accretion of binary-driven hypernovae". United States. https://doi.org/10.1088/0004-637X/812/2/100. https://www.osti.gov/servlets/purl/1329681.
@article{osti_1329681,
title = {Angular momentum role in the hypercritical accretion of binary-driven hypernovae},
author = {Becerra, L. and Cipolletta, F. and Fryer, Chris L. and Rueda, Jorge A. and Ruffini, Remo},
abstractNote = {Here, the induced gravitational collapse paradigm explains a class of energetic, ${E}_{{\rm{iso}}}\gtrsim {10}^{52}$ erg, long-duration gamma-ray bursts (GRBs) associated with Ic supernovae, recently named binary-driven hypernovae. The progenitor is a tight binary system formed of a carbon–oxygen (CO) core and a neutron star (NS) companion. The supernova ejecta of the exploding CO core trigger a hypercritical accretion process onto the NS, which reaches the critical mass in a few seconds, and gravitationally collapses to a black hole, emitting a GRB. In our previous simulations of this process, we adopted a spherically symmetric approximation to compute the features of the hypercritical accretion process. We here present the first estimates of the angular momentum transported by the supernova ejecta, ${L}_{{\rm{acc}}},$ and perform numerical simulations of the angular momentum transfer to the NS during the hyperaccretion process in full general relativity. We show that the NS (1) reaches either the mass-shedding limit or the secular axisymmetric instability in a few seconds depending on its initial mass, (2) reaches a maximum dimensionless angular momentum value, ${[{cJ}/({{GM}}^{2})]}_{{\rm{max}}}\approx 0.7$, and (3) can support less angular momentum than the one transported by supernova ejecta, ${L}_{{\rm{acc}}}\gt {J}_{{\rm{NS,max}}},$ hence there is an angular momentum excess that necessarily leads to jetted emission.},
doi = {10.1088/0004-637X/812/2/100},
journal = {The Astrophysical Journal (Online)},
number = 2,
volume = 812,
place = {United States},
year = {Mon Oct 12 00:00:00 EDT 2015},
month = {Mon Oct 12 00:00:00 EDT 2015}
}
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