@Article{RuffiniIBRBDEMPPW:2015:CaGR97,
author = "Ruffini, R. and Izzo, L. and Bianco, C. L. and Rueda, J. A. and
Barbarino, C. and Dereli, H. and Enderli, M. and Muccino, M. and
Penacchioni, Ana Virg{\'{\i}}nia and Pisani, G. B. and Wang,
Y.",
affiliation = "{Sapienza Universita di Roma} and {Sapienza Universita di Roma}
and {Sapienza Universita di Roma} and {Sapienza Universita di
Roma} and {Sapienza Universita di Roma} and {Universite de Nice
Sophia Antipolis} and {Sapienza Universita di Roma} and {Sapienza
Universita di Roma} and {Instituto Nacional de Pesquisas Espaciais
(INPE)} and {Sapienza Universita di Roma} and {Sapienza Universita
di Roma}",
title = "Induced gravitational collapse in the BATSE era: the case of GRB
970828",
journal = "Astronomy Reports",
year = "2015",
volume = "59",
number = "7",
pages = "626--638",
month = "July",
abstract = "Following the recently established {"}Binary-driven HyperNova{"}
(BdHN) model, we here interpret GRB 970828 in terms of the four
episodes typical of such a model. The {"}Episode 1,{"} up to 40 s
after the trigger time t (0), with a time varying thermal emission
and a total energy of E-iso,E-1st = 2.60 x 10(53) erg, is
interpreted as due to the onset of an hyper-critical accretion
process onto a companion neutron star, triggered by the companion
star, an FeCO core undergoing a SN explosion. The {"}Episode 2,{"}
observed up t (0) + 90 s, is interpreted as a canonical gamma ray
burst, with an energy of erg, a baryon load of B = 7x 10(-3) and a
bulk Lorentz factor at transparency of G = 142.5. From this
Episode 2, we infer that the GRB exploded in an environment with a
large average particle density aOE (c) n > a parts per thousand
103 particles/cm(3) and dense clouds characterized by typical
dimensions of (4-8) x 10(14) cm and delta n/n similar to 10. The
{"}Episode 3{"} is identified from t (0) +90 s all the way up to
10(5-6) s: despite the paucity of the early X-ray data, typical in
the BATSE, pre-Swift era, we find extremely significant data
points in the late X-ray afterglow emission of GRB 970828, which
corresponds to the ones observed in all BdHNe sources. The
{"}Episode 4,{"} related to the Supernova emission, does not
appear to be observable in this source, due to the presence of
darkening from the large density of the GRB environment, also
inferred from the analysis of the Episode 2.",
doi = "10.1134/S1063772915070094",
url = "http://dx.doi.org/10.1134/S1063772915070094",
issn = "1063-7729",
language = "en",
urlaccessdate = "27 abr. 2024"
}