During a compact binary merger involving at least one neutron star, a small fraction of the gravitational energy could be liberated in such a way to accelerate a small fraction (~ 10^-6) of the neutron star mass in an isotropic or quasi-isotropic way. In presence of certain conditions, a pair-loaded fireball can form, which undergoes accelerated expansion reaching relativistic velocities. As in the standard fireball scenario, internal energy is partly transformed into kinetic energy. At the photospheric radius, the internal radiation can escape, giving rise to a pulse that lasts for a time equal to the delay time since the merger. The subsequent interaction with the interstellar medium can then convert part of the remaining kinetic energy back into radiation in a weak isotropic afterglow at all wavelengths. This scenario does not require the presence of a jet: the associated isotropic prompt and afterglow emission should be visible for all NS-NS and BH-NS mergers within 90 Mpc, independent of their inclination. The prompt emission is similar to that expected from an off-axis jet, either structured or much slower than usually assumed (Gamma ~ 10), or from the jet cocoon. The predicted afterglow emission properties can discriminate among these scenarios

Salafia, O., Ghisellini, G., Ghirlanda, G. (2018). Jet-driven and jet-less fireballs from compact binary mergers. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 474(1), L7-L11 [10.1093/mnrasl/slx189].

Jet-driven and jet-less fireballs from compact binary mergers

Salafia, O;Ghisellini, G;Ghirlanda, G
2018

Abstract

During a compact binary merger involving at least one neutron star, a small fraction of the gravitational energy could be liberated in such a way to accelerate a small fraction (~ 10^-6) of the neutron star mass in an isotropic or quasi-isotropic way. In presence of certain conditions, a pair-loaded fireball can form, which undergoes accelerated expansion reaching relativistic velocities. As in the standard fireball scenario, internal energy is partly transformed into kinetic energy. At the photospheric radius, the internal radiation can escape, giving rise to a pulse that lasts for a time equal to the delay time since the merger. The subsequent interaction with the interstellar medium can then convert part of the remaining kinetic energy back into radiation in a weak isotropic afterglow at all wavelengths. This scenario does not require the presence of a jet: the associated isotropic prompt and afterglow emission should be visible for all NS-NS and BH-NS mergers within 90 Mpc, independent of their inclination. The prompt emission is similar to that expected from an off-axis jet, either structured or much slower than usually assumed (Gamma ~ 10), or from the jet cocoon. The predicted afterglow emission properties can discriminate among these scenarios
Articolo in rivista - Articolo scientifico
relativistic processes, stars:neutron, gamma-ray burst:general, gravitational waves
English
2018
474
1
L7
L11
none
Salafia, O., Ghisellini, G., Ghirlanda, G. (2018). Jet-driven and jet-less fireballs from compact binary mergers. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 474(1), L7-L11 [10.1093/mnrasl/slx189].
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/10281/174969
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