On the Induced Gravitational Collapse

¹ Dipartimento di Fisica and ICRA, Sapienza Università di Roma, P.le Aldo Moro 5, I–00185 Rome, Italy
² ICRANet, P.zza della Repubblica 10, I–65122 Pescara, Italy
³ ICRANet-Rio, Centro Brasileiro de Pesquisas Físicas, Rua Dr. Xavier Sigaud 150, 22290–180 Rio de Janeiro, Brazil
⁴ CCS-2, Los Alamos National Laboratory, Los Alamos, NM 87545

^* e-mail: laura.maarcela@icranet.com

Published online: 9 January 2018

Abstract

The induced gravitational collapse (IGC) paradigm has been applied to explain the long gamma ray burst (GRB) associated with type Ic supernova, and recently the Xray flashes (XRFs). The progenitor is a binary systems of a carbon-oxygen core (CO) and a neutron star (NS). The CO core collapses and undergoes a supernova explosion which triggers the hypercritical accretion onto the NS companion (up to 10^-2 M_⊙s^-1). For the binary driven hypernova (BdHNe), the binary system is enough bound, the NS reach its critical mass, and collapse to a black hole (BH) with a GRB emission characterized by an isotropic energy E_iso > 10⁵² erg. Otherwise, for binary systems with larger binary separations, the hypercritical accretion onto the NS is not sufficient to induced its gravitational collapse, a X-ray flash is produced with E_iso < 10⁵² erg. We’re going to focus in identify the binary parameters that limits the BdHNe systems with the XRFs systems.