On the induced gravitational collapse scenario of gamma-ray bursts associated with supernovae

Journal Article · Sat Dec 10 00:00:00 EST 2016 · The Astrophysical Journal (Online)

DOI:https://doi.org/10.3847/1538-4357/833/1/107· OSTI ID:1344359

Becerra, L. ^[1]; Bianco, C. L.  ^[1]; Fryer, C. L.  ^[2]; Rueda, J. A.  ^[3]; Ruffini, R. ^[3]

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

Following the induced gravitational collapse (IGC) paradigm of gamma-ray bursts (GRBs) associated with type Ib/c supernovae, we present numerical simulations of the explosion of a carbon–oxygen (CO) core in a binary system with a neutron-star (NS) companion. The supernova ejecta trigger a hypercritical accretion process onto the NS thanks to a copious neutrino emission and the trapping of photons within the accretion flow. We show that temperatures of 1–10 MeV develop near the NS surface, hence electron–positron annihilation into neutrinos becomes the main cooling channel leading to accretion rates of 10–9–$${10}^{-1}\,{M}_{\odot }$$ s–1 and neutrino luminosities of 10⁴³–10⁵² erg s^–1 (the shorter the orbital period the higher the accretion rate). We estimate the maximum orbital period, $${P}_{\max },$$ as a function of the NS initial mass, up to which the NS companion can reach by hypercritical accretion the critical mass for gravitational collapse leading to black hole formation. We then estimate the effects of the accreting and orbiting NS companion onto a novel geometry of the supernova ejecta density profile. We present the results of a $$1.4\times {10}^{7}$$ particle simulation which show that the NS induces accentuated asymmetries in the ejecta density around the orbital plane. We elaborate on the observables associated with the above features of the IGC process. We apply this framework to specific GRBs: we find that X-ray flashes (XRFs) and binary-driven hypernovae are produced in binaries with $$P\gt {P}_{\max }$$ and $$P\lt {P}_{\max },$$ respectively. As a result, we analyze in detail the case of XRF 060218.

• Research Organization: Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
• Sponsoring Organization: USDOE National Nuclear Security Administration (NNSA), Office of Defense Programs (DP)
• Grant/Contract Number: AC52-06NA25396
• OSTI ID: 1344359
• Report Number(s): LA-UR-16-24477; TRN: US1701159
• Journal Information: The Astrophysical Journal (Online), Vol. 833, Issue 1; ISSN 1538-4357
• Publisher: Institute of Physics (IOP)
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
astronomy and astrophysics
accretion
accretion disks
stars: black holes
gamma-ray burst: general
stars: neutron
supernovae: general