EPJ Web of Conferences 168, 01006 (2018)
https://doi.org/10.1051/epjconf/201816801006

The binary progenitors of short and long GRBs and their gravitational-wave emission

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 Université de Nice Sophia Antipolis, CEDEX 2, Grand Château Parc Valrose, Nice,
⁵ Unit of Nonlinear Physics and Mathematical Modeling, Università Campus Bio-Medico di Roma, Via A. del Portillo 21, I–00128 Rome, Italy
⁶ ICRA, Università Campus Bio-Medico di Roma, Via A. del Portillo 21, I–00128 Rome, Italy

^* e-mail: jorge.rueda@icra.it

Published online: 9 January 2018

Abstract

We have sub-classified short and long-duration gamma-ray bursts (GRBs) into seven families according to the binary nature of their progenitors. Short GRBs are produced in mergers of neutron-star binaries (NS-NS) or neutron star-black hole binaries (NS-BH). Long GRBs are produced via the induced gravitational collapse (IGC) scenario occurring in a tight binary system composed of a carbon-oxygen core (COcore) and a NS companion. The COcore explodes as type Ic supernova (SN) leading to a hypercritical accretion process onto the NS: if the accretion is sufficiently high the NS reaches the critical mass and collapses forming a BH, otherwise a massive NS is formed. Therefore long GRBs can lead either to NS-BH or to NS-NS binaries depending on the entity of the accretion. We discuss for the above compact-object binaries: 1) the role of the NS structure and the nuclear equation of state; 2) the occurrence rates obtained from X and gamma-rays observations; 3) the predicted annual number of detections by the Advanced LIGO interferometer of their gravitational-wave emission.