Photospheric emission in gamma-ray bursts

Pe’er, Asaf; Ryde, F.

doi:10.1142/9789813226609_0044

Cited by 4 publications

(3 citation statements)

References 184 publications

(332 reference statements)

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“…Although more detailed calculations performed by [364,365] have demonstrated that the internal-shock model which includes benchmark parameters (e.g., the bulk Lorentz factor Γ B = 300) is consistent with the upper limits obtained by IceCube, these results have posed more stringent constraints on the internal shocks model because there is a possible correlation between the bulk Lorentz factor Γ B and the GRB luminosity [366,367,368]. Instead, alternative scenarios in the context of the ultra-relativistic jet model are the photospheric emission model [369,370,371,372,373], and the Internal-Collision-induced MAgnetic Reconnection and Turbulence (ICMART) model [374,375]. Photospheric models assume that thermal energy stored in the jet is radiated as prompt emission at the Thomson photosphere [376,377,378], while ICMART models envisage that collisions between "mini-shells" in a Poynting-flux-dominated outflow distorts the ordered magnetic field lines in a run-away manner, which accelerates particles that then radiate synchrotron γ-ray photons at radii of ∼ 10 15 − 10 16 cm [374,375].…”

Section: Central-engine Models -Millisecond Magnetars Vs Collapsarsmentioning

confidence: 61%

The Observer’s Guide to the Gamma-Ray Burst Supernova Connection

Cano

Wang

Dai

et al. 2017

Advances in Astronomy

289

277

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In this review article we present an up-to-date progress report of the connection between long-duration (and their various sub-classes) gamma-ray bursts (GRBs) and their accompanying supernovae (SNe). The analysis presented here is from the point of view of an observer, with much of the emphasis placed on how observations, and the modelling of observations, have constrained what we known about GRB-SNe. We discuss their photometric and spectroscopic properties, their role as cosmological probes, including their measured luminosity−decline relationships, and how they can be used to measure the Hubble constant. We present a statistical analysis of their bolometric properties, and use this to determine the properties of the "average" GRB-SN: which has a kinetic energy of E K ≈ 2.5 × 10 52 erg (σ E K = 1.8 × 10 52 erg), an ejecta mass of M ej ≈ 6 M (σ M ej = 4 M ), a nickel mass of M Ni ≈ 0.4 M (σ M Ni = 0.2 M ), an ejecta velocity at peak light of v ≈ 20, 000 km s −1 (σ v ph = 8, 000 km s −1 ), a peak bolometric luminosity of L p ≈ 1×10 43 erg s −1 (σ Lp = 0.4×10 43 erg s −1 ), and it reaches peak bolometric light in t p ≈ 13 days (σ tp = 2.7 days). We discuss their geometry, as constrained from observations, and consider the various physical processes that are thought to power the luminosity of GRB-SNe, and whether differences exist between GRB-SNe and the SNe associated with ultra-long duration GRBs such as GRB 111209A/SN 2011kl. We discuss how observations of the environments of GRB-SNe further constrain the physical properties of their pre-explosion progenitor stars, and give a brief overview of the current theoretical paradigms of the central engines that produce the various types of GRB-SNe. Furthermore, we present an overview of the r-process, radioactively powered transients that have been photometrically associated with short-duration GRBs, and we conclude the review by discussing what additional research is needed to further our understanding of GRB-SNe, in particular the role of binary-formation channels and the connection of GRB-SNe with superluminous SNe. arXiv:1604.03549v2 [astro-ph.HE] 18 Jul 2016 1 A: Strong spectroscopic evidence. B: A clear light curve bump as well as some spectroscopic evidence resembling a GRB-SN. C: A clear bump consistent with other GRB-SNe at the spectroscopic redshift of the GRB. D: A bump, but the inferred SN properties are not fully consistent with other GRB-SNe or the bump was not well sampled or there is no spectroscopic redshift of the GRB. E: A bump, either of low significance or inconsistent with other GRB-SNe. * Denotes exact, K-corrected rest-frame filter observable. ‡ Values fixed during fit.k ands denote the filter-averaged luminosity (k) and stretch (s) factors relative to SN 1998bw.

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Section: Central-engine Models -Millisecond Magnetars Vs Collapsarsmentioning

confidence: 61%

The Observer’s Guide to the Gamma-Ray Burst Supernova Connection

Cano

Wang

Dai

et al. 2017

Advances in Astronomy

289

277

View full text Add to dashboard Cite

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“…Preece et al 1998b;Ghirlanda, Celotti & Ghisellini 2002; ⋆ E-mail: gabriele.ghisellini@inaf.it 2014; Yu et al, 2016). Rarely, the very hard low energy spectra have been reproduced with a thermal component: in a few cases with a pure black body spectrum (Ghirlanda, Celotti & Ghisellini 2004;Ghirlanda, Pescalli & Ghisellini 2013); more often with a power law or a Band model with the addition of a black body contribution (Ryde & Pe'er 2009;Ryde et al 2010;Guiriec et al 2011;Burgess et al 2014;Pe'er & Ryde 2017; but see Ghirlanda et al 2007).…”

Section: Introductionmentioning

confidence: 99%

Proton–synchrotron as the radiation mechanism of the prompt emission of gamma-ray bursts?

Ghisellini

Ghirlanda

Oganesyan

et al. 2020

A&A

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We discuss the new surprising observational results that indicate quite convincingly that the prompt emission of Gamma-Ray Bursts (GRBs) is due to synchrotron radiation produced by a particle distribution that has a low energy cut-off. The evidence of this is provided by the low energy part of the spectrum of the prompt emission, that shows the characteristic F ν ∝ ν 1/3 shape followed by F ν ∝ ν −1/2 up to the peak frequency. This implies that although the emitting particles are in fast cooling, they do not cool completely. This poses a severe challenge to the basic ideas about how and where the emission is produced, because the incomplete cooling requires a small value of the magnetic field, to limit synchrotron cooling, and a large emitting region, to limit the self-Compton cooling, even considering Klein-Nishina scattering effects. Some new and fundamental ingredient is required for understanding the GRBs prompt emission. We propose proton-synchrotron as a promising mechanism to solve the incomplete cooling puzzle.

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“…A similar mechanism operates in the cannonball model (Dado et al 2007) which advocates bulk Comptonisation as the primary source of GRB prompt emission. On the other hand, evidence of thermal photospheric emission has been reported in many cases of prompt GRB emission (Pe'er & Ryde 2016). This component, while potentially providing seed photons for Compton drag, would by itself contribute little to polarized emission and hence reduce the overall degree of polarisation.…”

Section: Polarisationmentioning

confidence: 99%

Astrosat CZT Imager Observations of GRB 151006a: Timing, Spectroscopy, and Polarization Study

Rao

Chand

Hingar

et al. 2016

ApJ

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AstroSat is a multi-wavelength satellite launched on 2015 September 28. The CZT Imager of AstroSat on its very first day of operation detected a long duration gamma-ray burst (GRB) namely GRB 151006A. Using the off-axis imaging and spectral response of the instrument, we demonstrate that CZT Imager can localise this GRB correct to about a few degrees and it can provide, in conjunction with Swift, spectral parameters similar to that obtained from Fermi /GBM. Hence CZT Imager would be a useful addition to the currently operating GRB instruments (Swift and Fermi ). Specifically, we argue that the CZT Imager will be most useful for the short hard GRBs by providing localisation for those detected by Fermi and spectral information for those detected only by Swift. We also provide preliminary results on a new exciting capability of this instrument: CZT Imager is able to identify Compton scattered events thereby providing polarisation information for bright GRBs. GRB 151006A, in spite of being relatively faint, shows hints of a polarisation signal at 100-300 keV (though at a low significance level). We point out that CZT Imager should provide significant time resolved polarisation measurements for GRBs that have fluence 3 times higher than that of GRB 151006A. We estimate that the number of such bright GRBs detectable by CZT Imager is 5 -6 per year. CZT Imager can also act as a good hard X-ray monitoring device for possible electromagnetic counterparts of Gravitational Wave events.

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Photospheric emission in gamma-ray bursts

Cited by 4 publications

References 184 publications

The Observer’s Guide to the Gamma-Ray Burst Supernova Connection

The Observer’s Guide to the Gamma-Ray Burst Supernova Connection

Proton–synchrotron as the radiation mechanism of the prompt emission of gamma-ray bursts?

Astrosat CZT Imager Observations of GRB 151006a: Timing, Spectroscopy, and Polarization Study

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