inferences from GRB 130427A, GRB 160509A, GRB 160625B, GRB 180728A, and GRB 190114C
J. A. Rueda (Author), Remo Ruffini (Author), Mile Karlica (Author), Rahim Moradi (Author), Yu Wang (Author)

Abstract

GRB 190114C is the first binary-driven hypernova (BdHN) fully observed from initial supernova (SN) appearance to the final emergence of the optical SN signal. It offers an unprecedented testing ground for the BdHN theory, which is here determined and further extended to additional gamma-ray bursts (GRBs). BdHNe comprise two subclasses of long GRBs, with progenitors a binary system composed of a carbon–oxygen star (COcore) and a neutron star (NS) companion. The COcore explodes as an SN, leaving at its center a newborn NS (νNS). The SN ejecta hypercritically accretes on both the νNS and the NS companion. BdHNe I are very tight binaries, where the accretion leads the companion NS to gravitationally collapse into a black hole (BH). In BdHN II, the accretion rate onto the NS is lower, so there is no BH formation. We observe the same afterglow structure for GRB 190114C and other selected examples of BdHNe I (GRB 130427A, GRB 160509A, GRB 160625B) and for BdHN II (GRB 180728A). In all cases, the afterglows are explained via the synchrotron emission powered by the νNS, and their magnetic field structures and their spin are determined. For BdHNe I, we discuss the properties of the magnetic field embedding the newborn BH, which was inherited from the collapsed NS and amplified during the gravitational collapse process, and surrounded by the SN ejecta.

Keywords

astrophysics;high energy astrophysical phenomena;cosmology;nongalactic astrophysics;general relativity;quantum cosmology;

Data

Language: English
Year of publishing:
Typology: 1.01 - Original Scientific Article
Organization: UNG - University of Nova Gorica
UDC: 52
COBISS: 22999555 Link will open in a new window
ISSN: 1538-4357
Views: 1921
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Other data

URN: URN:SI:UNG
Type (COBISS): Not categorized
Pages: str. 1-13
Volume: ǂVol. ǂ893
Issue: ǂno. ǂ2
Chronology: Apr. 2020
DOI: 10.3847/1538-4357/ab80b9
ID: 11900535
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