Evolution of an electron-positron plasma produced by induced gravitational collapse in binary-driven hypernovae

J. D. Melon Fuksman; L. Becerra; C. L. Bianco; M. Karlica; M. Kovacevic; R. Moradi; M. Muccino; G. B. Pisani; D. Primorac; J. A. Rueda; R. Ruffini; G. V. Vereshchagin; Y. Wang

doi:10.1051/epjconf/201816804009

EPJ

a
b
c
d
e
ap
st
h
plus
ds
pv
ti
qt
am
n

Proceedings

Open Access

EPJ Web of Conferences 168, 04009 (2018)
https://doi.org/10.1051/epjconf/201816804009

Evolution of an electron-positron plasma produced by induced gravitational collapse in binary-driven hypernovae

J. D. Melon Fuksman¹^,2^*, L. Becerra¹^,2, C. L. Bianco¹^,2, M. Karlica¹^,2^,3, M. Kovacevic¹^,2^,3, R. Moradi¹^,2, M. Muccino¹^,2, G. B. Pisani¹^,2, D. Primorac¹^,2, J. A. Rueda¹^,2^,4, R. Ruffini¹^,2^,3^,4, G. V. Vereshchagin¹^,2 and Y. Wang¹^,2

¹ Dipartimento di Fisica, Sapienza Università di Roma, Piazzale Aldo Moro 5, 00185 Rome, Italy
² ICRANet, Piazza della Repubblica 10, 65122 Pescara, Italy
³ Université de Nice Sophia Antipolis, CEDEX 2, Grand Château Parc Valrose, Nice, France
⁴ ICRANet-Rio, Centro Brasileiro de Pesquisas Físicas, Rua Dr. Xavier Sigaud 150, 22290–180 Rio de Janeiro, Brazil

^* e-mail: david.melon@icranet.org

Published online: 9 January 2018

Abstract

The binary-driven hypernova (BdHN) model has been introduced in the past years, to explain a subfamily of gamma-ray bursts (GRBs) with energies E_iso ≥ 10⁵² erg associated with type Ic supernovae. Such BdHNe have as progenitor a tight binary system composed of a carbon-oxigen (CO) core and a neutron star undergoing an induced gravitational collapse to a black hole, triggered by the CO core explosion as a supernova (SN). This collapse produces an optically-thick e⁺e^- plasma, which expands and impacts onto the SN ejecta. This process is here considered as a candidate for the production of X-ray flares, which are frequently observed following the prompt emission of GRBs. In this work we follow the evolution of the e⁺e^- plasma as it interacts with the SN ejecta, by solving the equations of relativistic hydrodynamics numerically. Our results are compatible with the Lorentz factors estimated for the sources that produce the flares, of typically Γ ≲ 4.

© The Authors, published by EDP Sciences, 2018

This is an Open Access article distributed under the terms of the Creative Commons Attribution License 4.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. (http://creativecommons.org/licenses/by/4.0/).