GRB 130427A AND SN 2013cq: A MULTI-WAVELENGTH ANALYSIS OF AN INDUCED GRAVITATIONAL COLLAPSE EVENT

Ruffini, Remo; Wang, Y.; Enderli, M.; Muccino, M.; Bianco, C. L.; Penacchioni, A. V.; Pisani, G. B.; Rueda, J. A.

doi:10.1088/0004-637x/798/1/10

Cited by 47 publications

(133 citation statements)

References 57 publications

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“…In both cases it starts after the P-GRB emission and it is coeval with the occurrence of the prompt emission [42]. Moreover, the restframe 0.1-100 GeV luminosities in BdHNe and S-GRBs share a common luminosity pattern, a precise power-law behavior with time ∝ t −1.2 [9,10,42,65,85]. These commonalities, in such different systems, as well as their energy requirements are naturally explained if we assume that the GeV emission originates by accretion processes in the newly-born BH [9,10].…”

Section: Discussionmentioning

confidence: 82%

“…BdHNe occur in tighter binaries (a < 10 11 cm), where the hypercritical accretion onto the companion NS leads to the formation of a BH [41] and, therefore, to the emission of the associated prolonged GeV emission (observable when inside the LAT field of view). Specific constant power-law behaviors are observed in their high energy GeV and Xrays luminosity light curves [9,46,47]. The out-states of BdHNe are νNS-BH binaries [41,42,48,49].…”

Section: Introductionmentioning

confidence: 92%

“…These three components are dubbed flare-plateauafterglow (FPA) phase [79]. During the early X-ray flare phase (typically at a rest-frame time of ∼ 10 2 s) an expanding thermal component has been observed in its spectrum [9,47,79]. The inferred radii are typically ∼ 10 12 -10 13 cm and they expand at mildly relativistic speed with Γ 4 [9,47,78,79].…”

Section: Xrfs and Bdhne In The Igc Paradigmmentioning

confidence: 99%

“…The use of the overlapping of the afterglows as a distance indicator has been explored by inferring the redshifts of GRB 101023 [34], and has been applied to predict the occurrence of the SN associated to GRB 130427A before its discovery [80], later confirmed by the observations [81][82][83][84]. In the IGC scenario, the FPA originates from the SN ejecta [9,79]. In BdHNe the SN ejecta experiences an energy injection from GRB emission leading to the occurrence of a broad-lined SN Ic [75] with a kinetic energy larger than that of the traditional SNe Ic.…”

Section: Xrfs and Bdhne In The Igc Paradigmmentioning

confidence: 99%

“…Thanks to the extensive data collected by γ-ray telescopes, such as AGILE, BATSE, BeppoSAX, Fermi, HETE-II, INTEGRAL, Konus/WIND and Swift, to more sofisticated time-resolved spectral analyses, and to the theoretical treatment of the fireshell model [6][7][8] it has become evident that both long and short bursts originate from binary progenitors and that they can be further subdivided into a variety of sub-classes, depending on the evolution of these binary systems [9][10][11].…”

Section: Introductionmentioning

confidence: 99%

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What can we learn from GRBs?

et al. 2018

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Abstract. We review our recent results on the classification of long and short gamma-ray bursts (GRBs) in different subclasses. We provide observational evidences for the binary nature of GRB progenitors. For long bursts the induced gravitational collapse (IGC) paradigm proposes as progenitor a tight binary system composed of a carbon-oxygen core (CO core ) and a neutron star (NS) companion; the supernova (SN) explosion of the CO core triggers a hypercritical accretion process onto the companion NS. For short bursts a NS-NS merger is traditionally adopted as the progenitor. We also indicate additional sub-classes originating from different progenitors: (CO core )-black hole (BH), BH-NS, and white dwarf-NS binaries. We also show how the outcomes of the further evolution of some of these sub-classes may become the progenitor systems of other sub-classes.

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Section: Discussionmentioning

confidence: 82%

Section: Introductionmentioning

confidence: 92%

Section: Xrfs and Bdhne In The Igc Paradigmmentioning

confidence: 99%

Section: Xrfs and Bdhne In The Igc Paradigmmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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What can we learn from GRBs?

et al. 2018

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Thermal emission in the early afterglow of gamma-ray bursts from their interaction with supernova ejecta

Ruffini

Vereshchagin

Wang

2017

A&A

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Context. A thermal X-ray component is observed in the early afterglow of some gamma-ray bursts. Possible explanations include shockwave breakout, relativistic photosphere, or emission from cocoon. The difficulties of these models are discussed. Aims. We propose an alternative model that attributes such a thermal component to the interaction of the gamma-ray burst outflow with a baryonic material near the gamma-ray burst source. Methods. The analytic model is based on relativistic energy-momentum conservation and a diffusion model for photons. The kinematic and observational properties of the supernova ejecta after the interaction are derived. In particular, the temperature and the duration of the thermal emission are obtained. Results. The model is applied to a prototypical GRB 090618 and other gamma-ray bursts associated with supernovae having thermal emission in the early afterglow. The mass of the baryonic material is found to be a few 10 −4 M , indicating that this material can be a small fraction of the supernova ejecta.

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The newborn black hole in GRB 191014C proves that it is alive

Moradi

Rueda

Ruffini

et al. 2021

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A multi-decade theoretical effort has been devoted to finding an efficient mechanism to use the rotational and electrodynamical extractable energy of a Kerr-Newman black hole (BH), to power the most energetic astrophysical sources such as gamma-ray bursts (GRBs) and active galactic nuclei. We show an efficient general relativistic electrodynamical process which occurs in the “inner engine” of a binary driven hypernova. The inner engine is composed of a rotating Kerr BH of mass M and dimensionless spin parameter α, a magnetic field of strength B0 aligned and parallel to the rotation axis, and a very low-density ionized plasma. Here, we show that the gravitomagnetic interaction between the BH and the magnetic field induces an electric field that accelerates electrons and protons from the environment to ultrarelativistic energies emitting synchrotron radiation. We show that in GRB 190114C the BH of mass M = 4.4 M⊙, α = 0.4, and B0 ≈ 4 × 1010 G can lead to a high-energy (≳GeV) luminosity of 1051 erg s−1. The inner engine parameters are determined by requiring (1) that the BH extractable energy explains the GeV and ultrahigh-energy emission energetics, (2) that the emitted photons are not subjected to magnetic-pair production, and (3) that the synchrotron radiation timescale agrees with the observed high-energy timescale. We find for GRB 190114C a clear jetted emission of GeV energies with a semi-aperture angle of approximately 60° with respect to the BH rotation axis.

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GRB 130427A AND SN 2013cq: A MULTI-WAVELENGTH ANALYSIS OF AN INDUCED GRAVITATIONAL COLLAPSE EVENT

Cited by 47 publications

References 57 publications

What can we learn from GRBs?

What can we learn from GRBs?

Thermal emission in the early afterglow of gamma-ray bursts from their interaction with supernova ejecta

The newborn black hole in GRB 191014C proves that it is alive

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