GRB 090618: a candidate for a neutron star gravitational collapse onto a black hole induced by a type Ib/c supernova

Izzo, L.; Rueda, J. A.; Ruffini, Remo

doi:10.1051/0004-6361/201219813

Cited by 51 publications

(71 citation statements)

References 36 publications

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“…Following the works of Rueda & Ruffini (2012) and Izzo et al (2012b), we suggest for the origin of GRB 110709B a binary system formed by a massive evolved star on the verge of an SN explosion and an NS. The early SN material expanding at non-relativistic velocities is then accreted by the NS companion at times longer than t 0,accr , when the material reaches the NS gravitational capture region.…”

Section: Nature Of the Progenitormentioning

confidence: 67%

“…Episode 1 lasts 100 s and episode 2 lasts 135 s. Particularly interesting is the fact that the X-ray observations started well before the second trigger time. The light curve and spectrum of this source share characteristics with GRB 090618 (Izzo et al 2012b), GRB 101023 (Penacchioni et al 2012), and GRB 970828 (Izzo et al 2012c). It has recently been shown that GRBs that show such distinct emissions, episodes 1 and 2, form a new family of GRBs, which are described by the IGC paradigm (Rueda & Ruffini 2012;Izzo et al 2012b).…”

Section: Discussionmentioning

confidence: 81%

“…The light curve and spectrum of this source share characteristics with GRB 090618 (Izzo et al 2012b), GRB 101023 (Penacchioni et al 2012), and GRB 970828 (Izzo et al 2012c). It has recently been shown that GRBs that show such distinct emissions, episodes 1 and 2, form a new family of GRBs, which are described by the IGC paradigm (Rueda & Ruffini 2012;Izzo et al 2012b). Within this scenario, the GRB originates in a binary system formed by a massive star on the verge of an SN and an NS close to its critical mass for the gravitational collapse to a BH.…”

Section: Discussionmentioning

confidence: 81%

“…The prototype for the IGC paradigm has recently been given in the analysis of GRB 090618 (Izzo et al 2012a), following the works of Rueda & Ruffini (2012) and Izzo et al (2012b). In this work we follow the same line and identify four different Article published by EDP Sciences A133, page 1 of 12 episodes in GRB 110709B.…”

Section: Introductionmentioning

confidence: 99%

“…For this, the induced gravitational collapse (IGC) paradigm was first introduced by Ruffini et al (2001b) and was subsequently analyzed in Ruffini et al (2007Ruffini et al ( , 2008; Rueda & Ruffini (2012), and Izzo et al (2012b). Recently, it has been shown that this process can indeed explain the coincidence between the SN and GRB emission, both from an observational and a theoretical point of view (Izzo et al 2012a;Penacchioni et al 2012).…”

Section: Introductionmentioning

confidence: 99%

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GRB 110709B in the induced gravitational collapse paradigm

Penacchioni

Ruffini

Bianco

et al. 2013

A&A

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Context. Gamma-ray burst (GRB) 110709B is the first source for which Swift-BAT was triggered twice, with a time separation of ∼10 min. The first emission (called here episode 1) lasted from 40 s before the first trigger time until 60 s after it. The second emission (hereafter episode 2) lasted from 35 s before the second trigger time until 100 s after it. These features reproduce those of GRB 090618, which has recently been interpreted within the induced gravitational collapse (IGC) paradigm. In line with this paradigm, we assume the progenitor to be a close binary system composed of the core of an evolved star and a neutron star (NS). The evolved star explodes as a supernova (SN) and ejects material that is partially accreted by the NS. We identify this process with episode 1. The accretion process accumulates more than the critical mass of the NS, which gravitationally collapses into a black hole (BH). This process leads to the GRB emission, episode 2. The two trigger episodes have for the first time provided the possibility to cover the X-ray emission observed by XRT both prior to and during the prompt phase of GRB 110709B. Aims. We analyze the spectra and time variability of episodes 1 and 2 and compute the relevant parameters of the binary progenitor, as well as the astrophysical parameters both in the SN and the GRB phase in the IGC paradigm. Methods. We performed a time-resolved spectral analysis of episode 1 by fitting the spectrum with a blackbody (BB) plus a power-law (PL) spectral model. From the BB fluxes and temperatures of episode 1 and the luminosity distance d L , we evaluated the evolution with time of the radius of the BB emitter, associated here to the evolution of the SN ejecta. We analyzed episode 2 within the fireshell model, identifying the proper GRB (P-GRB) and simulating the light curve and spectrum. We established the redshift to be z = 0.75, following the phenomenological methods described in the literature, and our analysis of the late X-ray afterglow. It is most remarkable that the determination of the cosmological redshift on the basis of scaling the late X-ray afterglow, which was already verified in GRB 090618 and GRB 101023, is again verified by this analysis. Results. We find for episode 1 a temperature of the BB component that evolves with time following a broken PL, with the slope of the PL at early times α = 0 (constant function) and the slope of the PL at late times β = −4 ± 2. The break occurs at t = 41.21 s. The total energy of episode 1 is E (1) iso = 1.42 × 10 53 erg. The total energy of episode 2 is E (2) iso = 2.43 × 10 52 erg. We find at transparency a Lorentz factor Γ ∼ 1.73 × 10 2 , laboratory radius of 6.04 × 10 13 cm, P-GRB observed temperature kT P−GRB = 12.36 keV, baryon load B = 5.7 × 10 −3 and P-GRB energy of E P−GRB = 3.44 × 10 50 erg. We find a remarkable coincidence of the cosmological redshift by scaling the XRT data and with three other phenomenological methods. Conclusions. We interpret GRB 110709B as a member of the IGC sources, together with G...

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Section: Nature Of the Progenitormentioning

confidence: 67%

Section: Discussionmentioning

confidence: 81%

Section: Discussionmentioning

confidence: 81%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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GRB 110709B in the induced gravitational collapse paradigm

Penacchioni

Ruffini

Bianco

et al. 2013

A&A

Self Cite

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The key role of BeppoSAX in the GRB history

Frontera

2019

Rend. Fis. Acc. Lincei

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Twenty years have already been elapsed from the BeppoSAX discovery of the first afterglow of a Gamma Ray Burst (GRB) in February 28, 1997. Thanks to this discovery, it was possible to unveil the 30 year mystery about GRB origin: GRBs are huge explosions in galaxies at cosmological distances. Starting from the first GRB detection with Vela satellites, I will review the main results obtained before BeppoSAX , the story of the BeppoSAX discovery of the GRB afterglow with the consequent cosmological distance determination, the main BeppoSAX results and those obtained after the BeppoSAX era until to nowadays with the still open problems and prospects.

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Novel distance indicator for gamma-ray bursts associated with supernovae

Pisani

Izzo

Ruffini

et al. 2013

A&A

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Context. It has been proposed that the temporal coincidence of a gamma-ray burst (GRB) and a type Ib/c supernova (SN) can be explained with the concept of induced gravitational collapse (IGC), induced by the matter ejected from an SN Ib/c accreting onto a neutron star (NS). The NS is expected to reach the critical mass necessary for it to collapse to a black hole (BH) and emit a GRB. We found a standard luminosity light curve behavior in the late-time X-ray emission of this subclass of GRBs. Aims. We test if this standard behavior in the luminosity found in this subclass of GRBs can become a redshift estimator of these sources. Methods. We selected a sample of GRBs that belong to this subclass of IGC GRBs associated to an SN (IGC GRB-SN sources). These sources have an isotropic energy E iso > 10 52 erg and their cosmological redshifts are in the range of z = 0.49−1.261. We focused on the corresponding X-ray luminosity light curves. Results. We find that all GRBs of the sample with measured redshift present a standard luminosity late-time light curve in the 0.3−10 keV rest-frame energy range. We used these results to estimate the GRB redshift of the sample without a measured redshift and found results consistent with other possible redshift indicators. Conclusions. The standard late-time X-ray luminosity light curve of all GRBs of the sample shows a common physical mechanism in this particular phase of the X-ray emission, possibly related to the creation of the NS from the SN process. This scaling law moreover represents strong evidence of very low or even absent beaming in this late phase of the X-ray afterglow emission process. This could be a fundamental tool for estimating the redshift of GRBs that belong to this subclass of events. We are currently expanding this subclass of GRBs to further verify the universal validity of this new redshift estimation method.

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GRB 090618: a candidate for a neutron star gravitational collapse onto a black hole induced by a type Ib/c supernova

Cited by 51 publications

References 36 publications

GRB 110709B in the induced gravitational collapse paradigm

GRB 110709B in the induced gravitational collapse paradigm

The key role of BeppoSAX in the GRB history

Novel distance indicator for gamma-ray bursts associated with supernovae

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