The Maximum Isotropic Equivalent Energy of Gamma-Ray Bursts

Dado, S.; Dar, Arnon

doi:10.3847/2041-8213/ac98c8

Cited by 2 publications

(2 citation statements)

References 27 publications

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“…In particular, two properties are evident: (i) the absence of relatively low luminosity GRBs with short FWHM min (bottom left corner of each panel) is clearly an observational bias; (ii) the absence of luminous GRBs with long FWHM min (top right corner of each panel) is an intrinsic propriety of GRBs and suggests the possible existence of a maximum radiated energy within a single pulse (e.g. Dado & Dar 2022). To better appreciate this possibility, in each panel we show a grid with constant isotropic-equivalent released energy values of a single pulse, roughly estimated as E (pulse) iso ≈ L p FWHM min .…”

Section: Peak Rate Vs Fwhm Minmentioning

confidence: 99%

GRB minimum variability timescale with Insight-HXMT andSwift

Camisasca

Guidorzi

Amati³

et al. 2023

A&A

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Context. There has been significant technological and scientific progress in our ability to detect, monitor and model the physics of gamma-ray bursts (GRBs) over the 50 years since their first discovery. However, the dissipation process thought to be responsible for their defining prompt emission is still unknown. Recent efforts have focused on investigating how the ultrarelativistic jet of the GRB propagates through the progenitor's stellar envelope, for different initial composition shapes, jet structures, magnetisation, and -consequently -possible energy dissipation processes. Study of the temporal variability -in particular the shortest duration of an independent emission episode within a GRB -may provide a unique way to discriminate the imprint of the inner engine activity from geometry and propagation related effects. The advent of new high-energy detectors with exquisite time resolution now makes this possible. Aims. We aim to characterise the minimum variability timescale (MVT) defined as the shortest duration of individual pulses that shape a light curve for a sample of GRBs in the keV-MeV energy range and test correlations with other key observables, such as the peak luminosity, the Lorentz factor, and the jet opening angle. We compare these correlations with predictions from recent numerical simulations for a relativistic structured -possibly wobbling -jet and assess the value of temporal variability studies as probes of prompt-emission dissipation physics. Methods. We used the peak detection algorithm mepsa to identify the shortest pulse within a GRB time history and preliminarily calibrated mepsa to estimate the full width half maximum (FWHM) duration. We then applied this framework to two sets of GRBs:

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Section: Peak Rate Vs Fwhm Minmentioning

confidence: 99%

GRB minimum variability timescale with Insight-HXMT andSwift

Camisasca

Guidorzi

Amati³

et al. 2023

A&A

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“…The most intense GRBs reaching close to E iso ∼ 10 55 erg (Abdo et al 2009;Greiner et al 2009;Tsvetkova et al 2017) and L iso ∼5 × 10 54 erg s −1 (Frederiks et al 2013;Svinkin et al 2021). An upper limit on GRB isotropic energy has recently been predicted (E iso ∼ 3.8 × 10 54 erg; Dado & Dar 2022), which, together with a strong cutoff of the E iso distribution above 1-3 × 10 54 erg, suggested from the analysis of Konus-WIND (KW) and Fermi Gamma-ray Burst Monitor (GBM)samples of GRBs with known redshifts (Atteia et al 2017;Tsvetkova et al 2017Tsvetkova et al , 2021, imply very rare detections of extremely energetic GRBs. Bright, nearby GRBs provide a unique opportunity to probe the central-engine physics, prompt emission, and afterglow emission mechanisms, as well as the GRB local environment.…”

Section: Introductionmentioning

confidence: 99%

Properties of the Extremely Energetic GRB 221009A from Konus-WIND and SRG/ART-XC Observations

Frederiks

Svinkin

Lysenko

et al. 2023

ApJL

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We report on Konus-WIND (KW) and Mikhail Pavlinsky Astronomical Roentgen Telescope – X-ray Concentrator (ART-XC) observations and analysis of a nearby GRB 221009A, the brightest γ-ray burst (GRB) detected by KW for >28 yr of observations. The prompt, pulsed phase of the burst emission lasts for ∼600 s and is followed by a steady power-law decay lasting for more than 25 ks. From the analysis of the KW and ART-XC light curves and the KW spectral data, we derive time-averaged spectral peak energy of the burst E p ≈ 2.6 MeV, E p at the brightest emission peak ≈ 3.0 MeV, the total 20 keV–10 MeV energy fluence of ≈0.22 erg cm−2, and the peak energy flux in the same band of ≈0.031 erg cm−2 s−1. The enormous observed fluence and peak flux imply, at redshift z = 0.151, huge values of isotropic energy release E iso ≈ 1.2 × 1055 erg (or ≳6.5 solar rest mass) and isotropic peak luminosity L iso ≈ 3.4 × 1054 erg s−1 (64 ms scale), making GRB 221009A the most energetic and one of the most luminous bursts observed since the beginning of the GRB cosmological era in 1997. The isotropic energetics of the burst fit nicely both “Amati” and “Yonetoku” hardness–intensity correlations for >300 KW long GRBs, implying that GRB 221009A is most likely a very hard, super-energetic version of a “normal” long GRB.

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The Maximum Isotropic Equivalent Energy of Gamma-Ray Bursts

Cited by 2 publications

References 27 publications

GRB minimum variability timescale with Insight-HXMT andSwift

GRB minimum variability timescale with Insight-HXMT andSwift

Properties of the Extremely Energetic GRB 221009A from Konus-WIND and SRG/ART-XC Observations

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