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The morphology of the X-ray afterglows and of the jetted GeV emission in long GRBs
High Energy Astrophysical Phenomena · Submitted 16 Mar 2021
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim 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.
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The abstract, sentence by sentence
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.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We recall evidence that long gamma-ray bursts (GRBs) have binary progenitors and give new examples. | background 0.64 | 0.27 | 0.09 | asserted 0.98 |
| s1 | Binary-driven hypernovae (BdHNe) consist of a carbon-oxygen core (CO$_{\rm core}$) and a neutron star (NS) companion. | background 1.00 | 0.11 | 0.04 | asserted 1.00 |
| s2 | 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. | background 0.76 | 0.23 | 0.19 | asserted 1.00 |
| s3 | 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. | contribution 0.80 | 0.95 | 0.08 | asserted 1.00 |
| s4 | 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. | contribution 0.45 | 0.94 | 0.15 | asserted 0.98 |
| s5 | 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. | result 0.86 | 0.92 | 0.08 | asserted 1.00 |
| s6 | 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. | interpretation 0.77 | 0.90 | 0.25 | asserted 0.87 |
| s7 | 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. | result 0.88 | 0.92 | 0.28 | asserted 1.00 |
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The paper
Original abstract
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.
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References
How the literature uses it
5 arXiv papers cite this in 15 sentences
Papers citing it · 10 sentences without a confident label
Builds on it 1 paper
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The aim of this article is to extend the treatment of Ref. 2019JCAP...03..044R on WD-WD mergers, and exploit the analogy with the synchrotron emission in the X-rays, optical and radio bands in the afterglow of long GRBs [ref] to determine the emission of WD-WD mergers across the electromagnetic spectrum.
The white dwarf binary merger model of GRB 170817A · Introduction · 0.85
Uses its data or values 1 paper
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In GRB 190114C, the $ν$NS-rise emission extends from $t_rf=0.79$ s to $t_rf=1.18$ s [ref] .
Evidence for the transition of a Jacobi ellipsoid into a Maclaurin spheroid in gamma-ray bursts · Sequence of BdHN physical phenomena and observables · 0.95
Cites it as background 2 papers
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A series of Episodes, corresponding to new different physical laws, take place on vastly different characteristic time scales ranging from quantum electrodynamics (QED) time scales of $10^-21$ s, to classical electrodynamics processes of $10^-14$ s, as well as to gravitational processes of $10^-6$ s, and to hydrodynamics timescales of $1$ s and of $10^7$ s, and the GRB source lifetime can indeed be as long as $10^17$ s, i.e. the Universe lifetime (see [ref] , and references therein).
Nature of the ultrarelativistic prompt emission phase of GRB 190114C · Introduction · 0.81
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Since the last decades, great progress has been made for understanding the GRB natures [ref] .
Gravo-thermal catastrophe in gravitational collapse and energy progenitor of Gamma-Ray Bursts · Introduction · 1.00
What it cites · 9 sentences without a confident label
Uses the method or tool of 1 paper
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We here apply the self-consistent solution already well tested in the case of GRB 130427A [ref] and GRB 190114C [ref] for determining the three parameters of the inner engine, namely the mass and spin of the BH as well as the strength of the surrounding magnetic field $B_0$.
The newborn black hole in GRB 191014C proves that it is alive · The determination of the mass and spin of the BH in BdHNe I · 0.88
Uses data or values from 1 paper
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Thanks to the Swift satellite, the number of detected GRBs increased rapidly to $1300$ sources with known redshifts [ref] .
The Open Universe survey of Swift-XRT GRB fields: a complete sample of HBL blazars · The largest ever multi-wavelength observational efforts · 0.88
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