Angular momentum role in the hypercritical accretion of binary-driven hypernovae
- Dipartimento di Fisica and ICRA, Sapienza Università di Roma, P.le Aldo Moro 5, I-00185 Rome (Italy)
- CCS-2, Los Alamos National Laboratory, Los Alamos, NM 87545 (United States)
The induced gravitational collapse paradigm explains a class of energetic, E{sub iso}≳10{sup 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{sub 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{sup 2})]{sub max}≈0.7, and (3) can support less angular momentum than the one transported by supernova ejecta, L{sub acc}>J{sub NS,max}, hence there is an angular momentum excess that necessarily leads to jetted emission.
- OSTI ID:
- 22882484
- Journal Information:
- Astrophysical Journal, Vol. 812, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Since 2009, the country of publication for this journal is the UK.; ISSN 0004-637X
- Country of Publication:
- United Kingdom
- Language:
- English
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