Analysis of GRB 080319b and GRB 050904 Within the Fireshell Model: Evidence for a Broader Spectral Energy Distribution

Patricelli, B.; Bernardini, M. G.; Bianco, C. L.; Caito, Letizia; Barros, Gustavo; Izzo, L.; Ruffini, Remo; Vereshchagin, Gregory

doi:10.1088/0004-637x/756/1/16

Cited by 27 publications

(35 citation statements)

References 138 publications

(282 reference statements)

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“…The selected prototypes of Episode 2 emission have isotropic energies ranging from E iso = 1.60 × 10 53 erg in GRB 970828 (Ruffini et al 2015c), to E iso = 1.32×10 54 erg in GRB 080319B (Patricelli et al 2012). The amount of baryonic matter loaded before the P-GRB emission, the baryon load B ≡ M B c 2 /E tot e + e − , where E tot e + e − is the pair plasma energy and M B the engulfed baryon mass, is in the range from B = 1.98 × 10 −3 for GRB 090618 (Izzo et al 2012c), to B = 7.0 × 10 −3 in GRB 970828 (Ruffini et al 2015c).…”

Section: Prototypesmentioning

confidence: 99%

ON THE CLASSIFICATION OF GRBs AND THEIR OCCURRENCE RATES

Ruffini

Rueda

Muccino

et al. 2016

ApJ

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238

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There is mounting evidence for the binary nature of the progenitors of gamma-ray bursts (GRBs). For a long GRB, the induced gravitational collapse (IGC) paradigm proposes as progenitor, or "in-state", a tight binary system composed of a carbon-oxygen core (CO core ) undergoing a supernova (SN) explosion which triggers hypercritical accretion onto a neutron star (NS) companion. For a short GRB, a NS-NS merger is traditionally adopted as the progenitor. We divide long and short GRBs into two sub-classes, depending on whether or not a black hole (BH) is formed in the merger or in the hypercritical accretion process exceeding the NS critical mass. For long bursts, when no BH is formed we have the sub-class of X-ray flashes (XRFs), with isotropic energy E iso 10 52 erg and rest-frame spectral peak energy E p,i 200 keV. When a BH is formed we have the sub-class of binary-driven hypernovae (BdHNe), with E iso 10 52 erg and E p,i 200 keV. In analogy, short bursts are similarly divided into two sub-classes. When no BH is formed, short gamma-ray flashes (S-GRFs) occur, with E iso 10 52 erg and E p,i 2 MeV. When a BH is formed, the authentic short GRBs (S-GRBs) occur, with E iso 10 52 erg and E p,i 2 MeV. We give examples and observational signatures of these four sub-classes and their rate of occurrence. From their respective rates it is possible that "in-states" of S-GRFs and S-GRBs originate from the "out-states" of XRFs. We indicate two additional progenitor systems: white dwarf-NS and BH-NS. These systems have hybrid features between long and short bursts. In the case of S-GRBs and BdHNe evidence is given of the coincidence of the onset of the high energy GeV emission with the birth of a Kerr BH.

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Section: Prototypesmentioning

confidence: 99%

ON THE CLASSIFICATION OF GRBs AND THEIR OCCURRENCE RATES

Ruffini

Rueda

Muccino

et al. 2016

ApJ

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238

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“…(A color version of this figure is available in the online journal.) (Patricelli et al 2012), given by…”

Section: The Extended Afterglow Emissionmentioning

confidence: 99%

“…(A color version of this figure is available in the online journal.) Table 4 The Results of the Spectral Analysis of the P-GRB (from T 0 − 0.016 s to T 0 + 0.080 s, Best-fit BB+Band Model) and the Extended Afterglow (from T 0 + 0.080 s to T 0 + 0.368 s, Best-fit Band Model) of GRB 090227B in the Energy Range 8 keV-40 MeV (keV) (1.34 ± 0.01) × 10 3 z 1.61 ± 0.14 n (particles cm −3 ) ( 1 .90 ± 0.20) × 10 −5 δn/n 0.82 ± 0.11 (8-1000 keV) of GRB 090227B and in Figure 12 (left panel) we show the corresponding spectrum in the early ∼0.4 s of the emission, using the spectral model described by Equation (1) (Patricelli et al 2012). The simulation of the extended afterglow starts T a − T 0 ∼ 0.017 s after the Trigtime T 0 .…”

Section: Intervalmentioning

confidence: 99%

GRB 090227b: The Missing Link Between the Genuine Short and Long Gamma-Ray Bursts

Muccino¹,

Ruffini²,

Bianco³

et al. 2013

ApJ

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The time-resolved spectral analysis of GRB 090227B, made possible by the Fermi-GBM data, allows us to identify in this source the missing link between the genuine short and long gamma-ray bursts (GRBs). Within the Fireshell model of the GRBs we predict genuine short GRBs: bursts with the same inner engine of the long bursts but endowed with a severely low value of the baryon load, B 5 × 10 −5 . A first energetically predominant emission occurs at the transparency of the e + e − plasma, the Proper-GRB (P-GRB), followed by a softer emission, the extended afterglow. The typical separation between the two emissions is expected to be of the order of 10 −3 -10 −2 s. We identify the P-GRB of GRB 090227B in the first 96 ms of emission, where a thermal component with the temperature kT = (517 ± 28) keV and a flux comparable with the non-thermal part of the spectrum is observed. This non-thermal component as well as the subsequent emission, where there is no evidence for a thermal spectrum, is identified with the extended afterglow. We deduce a theoretical cosmological redshift z = 1.61 ± 0.14. We then derive the total energy E tot e + e − = (2.83 ± 0.15) × 10 53 erg, the baryon load B = (4.13 ± 0.05) × 10 −5 , the Lorentz Γ factor at transparency Γ tr = (1.44 ± 0.01) × 10 4 , and the intrinsic duration Δt ∼ 0.35 s. We also determine the average density of the circumburst medium (CBM), n CBM = (1.90 ± 0.20) × 10 −5 particles cm −3 . There is no evidence of beaming in the system. In view of the energetics and of the baryon load of the source, as well as of the low interstellar medium and of the intrinsic timescale of the signal, we identify the GRB progenitor as a binary neutron star. From the recent progress in the theory of neutron stars, we obtain masses of the stars m 1 = m 2 = 1.34 M and their corresponding radii R 1 = R 2 = 12.24 km and thickness of their crusts ∼0.47 km, consistent with the above values of the baryon load, of the energetics and of the time duration of the event.

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“…2 (left panel) has been simulated by using a CBM number density distribution with an average value of n CBM = (4.7 ± 1.2) × 10 −5 cm −3 . The corresponding spectrum 14 , is plotted in Fig. 2 (right panel).…”

Section: −5mentioning

confidence: 99%

GRB 140619B: A short GRB from a binary neutron star merger leading to black hole formation

Muccino

Ruffini

Oliveira

et al. 2017

The Fourteenth Marcel Grossmann Meeting

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For short gamma-ray bursts (GRBs), double neutron star (NS) mergers are traditionally adopted as progenitors. We propose a classification of short bursts into two sub-classes: short gamma-ray flashes (S-GRFs) with isotropic energy E iso 10 52 erg and rest-frame spectral peak energy E p,i 2 MeV, when the merger leads to a very massive NS (MNS), and the authentic short GRBs (S-GRBs) with E iso 10 52 erg and E p,i 2 MeV, when a black hole (BH) is formed. Evidences for the BH formation in S-GRBs are provided by the observed high energy 0.1-100 GeV emission after the GRB emission from the e + e − -plasma transparency (P-GRB); in S-GRFs, leading to MNS, this emission is never observed. Both these sub-classes fulfill the E p,i -E iso relation for short GRBs. We present here the recently identified S-GRB 140619B. From the spectral analysis of the early ∼ 0.2 s, we infer an observed P-GRB temperature kT = (324 ± 33) keV, a theoretically derived redshift z = 2.67 ± 0.37, a total burst energy E tot e + e − = (6.03 ± 0.79) × 10 52 erg, and a baryon load B = (5.52 ± 0.73) × 10 −5 . We also estimate the emission of gravitational waves (GWs) of the progenitor NS-NS merger. Including all the S-GRBs so far identified, the observed rate of these sources is ρ 0 = 3.5 +3.4 −2.0 × 10 −4 Gpc −3 yr −1 .

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Analysis of GRB 080319b and GRB 050904 Within the Fireshell Model: Evidence for a Broader Spectral Energy Distribution

Cited by 27 publications

References 138 publications

ON THE CLASSIFICATION OF GRBs AND THEIR OCCURRENCE RATES

ON THE CLASSIFICATION OF GRBs AND THEIR OCCURRENCE RATES

GRB 090227b: The Missing Link Between the Genuine Short and Long Gamma-Ray Bursts

GRB 140619B: A short GRB from a binary neutron star merger leading to black hole formation

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