Theories of Gamma-Ray Bursts

By P. Mészáros. 2001

407 citations recorded by the source corpus.

▪ Abstract The gamma ray burst phenomenon is reviewed from a theoretical point of view, with emphasis on the fireball shock scenario of the prompt emission and the longer wavelength afterglow. Rece...

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/d071887583ced836e00ea215da2edae1faec0d11

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Citations in the corpus

Short-Duration Gamma-Ray Bursts (2013, background): “…connection, and afterglowtheory (van Paradijs, Kouveliotou & Wijers 2000); comprehensive reviews of the prompt emission and afterglow theory (Mészáros 2002, Piran 2004); a detailed review of the long GRB-supernova connection (Woosley & Bloom 2006); a preliminary review of short GRBs,…”
Neutrino-dominated accretion flows as the central engine of gamma-ray bursts (2017, background): “…which may be related to GRBs. GRBs are extremely energetic transient events in the Universe and isotropically distributed over the sky (see e.g., Mészáros 2002; Zhang & Mészáros 2004; Zhang 2007; Gehrels et al. 2009; Kumar & Zhang 2015; Wang et al. 2015 for reviews), which are sorted into…”
High-resolution calculations of merging neutron stars - III. Gamma-ray bursts (2003, background): “…some general ways by which gravity, angular momentum and electromagnetic field could conspire to power GRBs (see e.g. Narayan et al. 1992; Thompson & Duncan 1993; Usov 1992, 1994; Mészáros & Rees 1997; Katz 1997; for a more complete bibliography see the reviews of Piran 1999 and Mészáros 2002).”
Gamma-ray burst afterglows (2006, methodology): “…budget is needed (the injection energy has to be at least comparable to that already in the blastwave in order to have any significant injection signature, Zhang & Mészáros 2002), the internal model only demands a small fraction of the prompt emission energy to account for the distinct flares.”
The signature of supernova ejecta in the X-ray afterglow of the γ-ray burst 011211 (2002, methodology): “We fitted ionized reflection models(17) to the data for two cases: (1) where the walls of the stellar envelope subtend 2p sr solid angle to the X-ray source; (2) where the emission arises purely from the scattered X-ray flux, with no continuum emission.”
REM observations of GRB 060418 and GRB 060607A: the onset of the afterglow and the initial fireball Lorentz factor determination (2006, background): “The short variability timescales, coupled with the nonthermal GRB spectra, indeed imply that the sources emitting GRBs have a highly relativistic motion (Ruderman 1975; Fenimore et al. 1993; Piran 2000; Lithwick & Sari 2001), to avoid suppression of the high-energy photons due to pair production.”
Swift observations of the very intense flaring activity of Mrk 421 during 2006. I. Phenomenological picture of electron acceleration and predictions for MeV/GeV emission (2009, background): “From the observational side, we note that Waxman (1997) and Mészáros (2002), studying the the afterglow X-ray emission of γ−ray bursts (GRB), inferred an electron distribution index of s 2.3 ± 0.1.”
The late time evolution of gamma-ray bursts: ending hyperaccretion and producing flares (2006, unknown): “…for the subsequent production of a baryon-poor fireball [e.g., Fuller, Pruet & Abazajian (2000); Beloborodov (2003); Vlahakis & Königl (2003); Mészáros (2002)], or a magnetically dominated “cold fireball” [Lyutikov & Blandford (2002)], though the specific toroidal magnetic field geometry…”
The Cooling Behavior of Thermal Pulses in Gamma-Ray Bursts (2004, background): “For instance, for the Fermi type of particle acceleration in relativistic shocks, p 2:2 (Mészáros 2002).”
Mergers of Neutron Star-Black Hole Binaries with Small Mass Ratios: Nucleosynthesis, Gamma-Ray Bursts, and Electromagnetic Transients (2005, background): “…central engines of gamma- ray bursts (GRBs) already two decades ago, they have been mentioned in Paczyński (1986) and Goodman et al. (1987) and discussed in more detail by Eichler et al. (1989) (for a more complete bibliography we refer to existing reviews, e.g. Meszaros 2002 or Piran 2005).”
General relativistic magnetohydrodynamic simulations of the jet formation and large-scale propagation from black hole accretion systems (2006, methodology): “However, by the radius simulated, the Lorentz factor is not yet large enough for the standard GRB internal shock model to be efficient (Kobayashi et al. 1997; Mészáros 2002; Ghirlanda et al. 2003; Piran 2005).”
Is Thermal Emission in Gamma-Ray Bursts Ubiquitous? (2005, background): “For the synchrotron, internal-shock model one expects E p ∝ Γ −2 L 1/2 t −1 v (e.g. Zhang & Mészáros (2002)), where t v is the typical variability time scale.”
The Ep,i–Eiso correlation in gamma-ray bursts: updated observational status, re-analysis and main implications (2006, background): “…which is currently the subject of many theoretical works, is that a substantial contribution to prompt radiation of GRBs comes from direct or Comptonized thermal emission from the photosphere of the fireball (Zhang & Mészáros 2002; Ryde 2005; Rees & Meśzaŕos 2005; Ramirez–Ruiz 2005).”
The Observable Effects of a Photospheric Component on GRB and XRF Prompt Emission Spectrum (2005, background): “The prompt emission from gamma-ray bursts (GRB’s) is believed to arise from the prompt dissipation of a substantial fraction of the bulk kinetic energy of a relativistic outflow, originating from a central compact object (for reviews, see Mészáros 2002; Waxman 2003; Piran 2004).”
Probing the cosmic reionization history and local environment of gamma‐ray bursts through radio dispersion (2003, background): “…as incoherent synchrotron emission from electrons accelerated by a relativistic blastwave decelerating in the ambient medium (Paczyński & Rhoads 1993, Katz 1994, Mészáros & Rees 1997, Sari, Piran & Narayan 1998; see Piran 1999, van Paradijs et al. 2000, Mészáros 2002 for reviews).”
The physics of core-collapse supernovae (2005, background): “GRBs — intense flashes of gamma-rays lasting about 20 s and coming from cosmological distances — are produced by highly relativistic collimated outflows (with Lorentz factors Γ =(1−( u / c 2−1/2>200 , where u is the outflow velocity”