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

• Published in: arXiv.org
• Main Authors: Ruffini, R, Moradi, R, Rueda, J A, L Li, Sahakyan, N, Y -C Chen, Wang, Y, Aimuratov, Y, Becerra, L, Bianco, C L, Cherubini, C, Filippi, S, Karlica, M, Mathews, G J, Muccino, M, Pisani, G B, Xue, S S
• Format: Paper Journal Article
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 16.03.2021
• Subjects: Afterglows; Alpha rays; Binary stars; Black holes; Boresights; Carbon monoxide; Companion stars; Deposition; Emission analysis; Evolution; Gamma ray bursts; Gamma rays; Luminosity; Morphology; Neutron stars; Physics - General Relativity and Quantum Cosmology; Physics - High Energy Astrophysical Phenomena; Progenitors (astrophysics); Spectrum analysis; Three dimensional analysis
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.2103.09142

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.