The binary progenitors of short and long GRBs and their gravitational-wave emission
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
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Published online: 9 January 2018
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.
© The Authors, published by EDP Sciences, 2018
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