On the Universal Late X-Ray Emission of Binary-Driven Hypernovae and Its Possible Collimation

Pisani, G. B.; Ruffini, Remo; Aimuratov, Y.; Bianco, C. L.; Moradi, R.; Muccino, M.; Penacchioni, A. V.; Rueda, J. A.; Shakeri, Soroush; Wang, Y.

doi:10.3847/1538-4357/833/2/159

Cited by 12 publications

(26 citation statements)

References 47 publications

(120 reference statements)

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“…In Pisani et al (2016), we present an "enlarged sample" (ES) of 161 BdHNe observed up to the end of 2015. In this work we analysed the signatures contained in the LXREs at t rf 10 4 s, where t rf is the rest-frame time after the initial GRB explosion.…”

Section: Towards a First Catalog Of Binary-driven Hypernovaementioning

confidence: 99%

“…Starting from the GS originally presented in Pisani et al (2013), in Pisani et al (2016) we have built a new sample of BdHNe, which we called "enlarged sample" (ES), under the following selection criteria:…”

Section: The First Enlarged Sample Of Bdhnmentioning

confidence: 99%

“…We collected 161 sources, satisfying our criteria, which cover 11 years of Swift/XRT observations, up to the end of 2015, see Table 2 of Pisani et al (2016). The E iso of each source has been estimated using the observed redshift z together with the best-fit parameters of the EPJ Web of Conferences 168, 04002 (2018) https://doi.org/10.1051/epjconf/201816804002…”

Section: The First Enlarged Sample Of Bdhnmentioning

confidence: 99%

“…Moreover, there is no evidence for a correlation between the LXRE power-law behavior and the isotropic energy radiated by the source during the GRB prompt radiation (for details, see Pisani et al 2016). …”

Section: Going To the Rest-framementioning

confidence: 99%

“…In Pisani et al (2016), we also proposed to reduce the spread of the LXRE power laws within the ES by introducing a collimation effect in the emission mechanism. In fact, if such a process is not isotropic, our estimates for the LXRE luminosities are actually overestimations of the intrinsic ones.…”

Section: Collimationmentioning

confidence: 99%

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The first ICRANet catalog of binary-driven hypernovae

et al. 2018

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In a series of recent publications, scientists from ICRANet, led by professor Remo Ruffini, have reached a novel comprehensive picture of gamma-ray bursts (GRBs) thanks to their development of a series of new theoretical approaches. Among those, the induced gravitational collapse (IGC) paradigm explains a class of energetic, long-duration GRBs associated with Ib/c supernovae (SN), recently named binary-driven hypernovae (BdHNe). BdHNe have a well defined set of observational features which allow to identify them. Among them, the main two are: 1) long duration of the GRB explosion, namely larger than 2 s in the rest frame; 2) a total energy, released in all directions by the GRB explosion, larger than 10 52 ergs. A striking result is the observation, in the BdHNe sources, of a universal late time power-law decay in the X-rays luminosity after 10 4 s, with typical decaying slope of ∼ 1.5. This leads to the possible establishment of a new distance indicator having redshift up to z ∼ 8. Thanks to this novel theoretical and observational understanding, it was possible for ICRANet scientists to build the firstst BdHNe catalog, composed by the 345 BdHNe identified up to the end of 2016. Keywords: supernovae: general -binaries: general -gamma-ray burst: general -stars: neutron TOWARDS A FIRST CATALOG OF BINARY-DRIVEN HYPERNOVAEThe first observations by the BATSE instrument on board the Compton γ-ray Observatory satellite have evidenced what has later become known as the prompt radiation of GRBs. On the basis of their hardness as well as their duration, GRBs were initially classified into short and long in an epoch when their cosmological nature was still being debated (Mazets et al. 1981;Klebesadel 1992;Dezalay et al. 1992;Kouveliotou et al. 1993;Tavani 1998).The advent of the BeppoSAX satellite (Boella et al. 1997) introduced a new approach to GRBs by introducing joint observations in the X-rays and γ-rays thanks to its instruments: the Gamma-ray Burst Monitor (40-700 keV), the Wide Field Cameras (2-26 keV), and the Narrow Field Instruments (2-10 keV). The unexpected discovery of a well separate component in the GRB soon appeared: the afterglow, namely a radiation lasting up to 10 5 -10 6 s after the emission of the prompt radiation (see Costa et al. 1997a,b;Frontera et al. 1998Frontera et al. , 2000de Pasquale et al. 2006). Beppo-SAX clearly indicated the existence of a power law behavior in the late X-ray emission (LXRE).The coming of the Swift satellite (Gehrels et al. 2004;Evans et al. 2007Evans et al. , 2010, significantly extending the ob- servation energy band to the X-ray band thanks to its X-ray Telescope (XRT band: 0.3-10 keV), has allowed us for the first time to uncover the unexplored region between the end of the prompt radiation and the power-law late X-ray behavior discovered by BeppoSAX : in some long GRBs, a steep decay phase was observed leading to a plateau followed then by a typical LXRE power law behavior (Evans et al. 2007(Evans et al. , 2010.Recently, Pisani et al. (2013) noticed the unex...

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Section: Towards a First Catalog Of Binary-driven Hypernovaementioning

confidence: 99%

Section: The First Enlarged Sample Of Bdhnmentioning

confidence: 99%

Section: The First Enlarged Sample Of Bdhnmentioning

confidence: 99%

Section: Going To the Rest-framementioning

confidence: 99%

Section: Collimationmentioning

confidence: 99%

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The first ICRANet catalog of binary-driven hypernovae

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

Ruffini

Moradi

Rueda

et al. 2021

Monthly Notices of the Royal Astronomical Society

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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 (COcore) and a neutron star (NS) companion. For binary periods ∼5 min, the COcore 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 (νNS), 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) AX, αX = 1.48 ± 0.32, and 3) the νNS spin time-evolution. We infer a) AGeV, αGeV = 1.19 ± 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 ≈60○ from the normal to the orbital plane. We deduce BH masses 2.3–8.9 M⊙ 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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On the Universal Late X-Ray Emission of Binary-Driven Hypernovae and Its Possible Collimation

Cited by 12 publications

References 47 publications

The first ICRANet catalog of binary-driven hypernovae

The first ICRANet catalog of binary-driven hypernovae

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

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

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