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Article Dans Une Revue Monthly Notices of the Royal Astronomical Society Année : 2021

The morphology of the X-ray afterglows and of the jetted GeV emission in long GRBs

R. Moradi
  • Fonction : Auteur
J.A. Rueda
  • Fonction : Auteur
L. Li
  • Fonction : Auteur
N. Sahakyan
Y.-C Chen
  • Fonction : Auteur
Y. Wang
  • Fonction : Auteur
Y. Aimuratov
  • Fonction : Auteur
L. Becerra
  • Fonction : Auteur
C.L. Bianco
  • Fonction : Auteur
C. Cherubini
  • Fonction : Auteur
S. Filippi
  • Fonction : Auteur
M. Karlica
  • Fonction : Auteur
G.J. Mathews
  • Fonction : Auteur
M. Muccino
  • Fonction : Auteur
G.B. Pisani
  • Fonction : Auteur
S.S. Xue
  • Fonction : Auteur

Résumé

We recall evidence that long gamma-ray bursts (GRBs) have binary progenitors and give new examples. Binary-driven hypernovae (BdHNe) consist of a carbon-oxygen core (CO$_{\rm core}$) and a neutron star (NS) companion. For binary periods $\sim 5$ min, the CO$_{\rm core}$ collapse originates the subclass BdHN I characterized by: 1) an energetic supernova (the "SN-rise"); 2) a black hole (BH), born from the NS collapse by SN matter accretion, leading to a GeV emission with luminosity $L_{\rm GeV} = A_{\rm GeV}\,t^{-\alpha_{\rm GeV}}$, observed only in some cases; 3) a new NS ($\nu$NS), born from the SN, originating the X-ray afterglow with $L_X = A_{\rm X}\,t^{-\alpha_{\rm X}}$, observed in all BdHN I. We record $378$ sources and present for four prototypes GRBs 130427A, 160509A, 180720B and 190114C: 1) spectra, luminosities, SN-rise duration; 2) $A_X$, $\alpha_X=1.48\pm 0.32$, and 3) the $\nu$NS spin time-evolution. We infer a) $A_{\rm GeV}$, $\alpha_{\rm GeV}=1.19 \pm 0.04$; b) the BdHN I morphology from time-resolved spectral analysis, three-dimensional simulations, and the GeV emission presence/absence in $54$ sources within the Fermi-LAT boresight angle. For $25$ sources, we give the integrated and time-varying GeV emission, $29$ sources have no GeV emission detected and show X/gamma-ray flares previously inferred as observed along the binary plane. The $25/54$ ratio implies the GeV radiation is emitted within a cone of half-opening angle $\approx 60^{\circ}$ from the normal to the orbital plane. We deduce BH masses $2.3$-$8.9~M_\odot$ and spin $0.27$-$0.87$ by explaining the GeV emission from the BH energy extraction, while their time evolution validates the BH mass-energy formula.

Dates et versions

hal-03186184 , version 1 (30-03-2021)

Identifiants

Citer

R. Ruffini, R. Moradi, J.A. Rueda, L. Li, N. Sahakyan, et al.. The morphology of the X-ray afterglows and of the jetted GeV emission in long GRBs. Monthly Notices of the Royal Astronomical Society, 2021, ⟨10.1093/mnras/stab724⟩. ⟨hal-03186184⟩

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