X-Ray-rich Gamma-Ray Bursts, Photospheres, and Variability

By P. Mészáros, E. Ramirez-Ruiz, Martin J. Rees, B. Z. P. S. U. IoA, C. University. 2002

145 citations recorded by the source corpus.

We investigate the relationship between the quasi-thermal baryon-related photosphere in relativistic outflows and the internal shocks arising outside them, which out to a limiting radius may be able to create enough pairs to extend the optically thick region. Variable gamma-ray light curves are likely to arise outside this limiting pair-forming shock radius, while X-ray excess bursts may arise from shocks occurring below it; a possible relation to X-ray flashes is discussed. This model leads to a simple physical interpretation of the observational gamma-ray variability-luminosity relation.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/55d912b3216a755495fa8e74fa2ee30fce38236a

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In Astronomy and Astrophysics

1. Bing Zhang
2. Pawan Kumar
3. E. Liang
4. E. Berger
5. B. Metzger
6. Binbin Zhang
7. E. Nakar
8. A. Pe’er

In Nuclear and High Energy Physics

1. Bing Zhang
2. Pawan Kumar
3. A. Pe’er
4. F. Ryde
5. Stephan Rosswog
6. E. Orlando
7. P. Mészáros
8. C. Dermer

Citations in the corpus

• GRB110721A: AN EXTREME PEAK ENERGY AND SIGNATURES OF THE PHOTOSPHERE (2012, background): “It was, however, realized that the photospheric emission should be accompanied by nonthermal emission from optically thin regions (e.g. Mészáros et al. 2002), and that the photospheric emission can be enhanced and modified from a Planck function by energy dissipation at moderate optical depths…”
• QUASI-BLACKBODY COMPONENT AND RADIATIVE EFFICIENCY OF THE PROMPT EMISSION OF GAMMA-RAY BURSTS (2008, background): “…that the purely nonthermal emission models face are readily alleviated by introducing an additional optically thick thermal (blackbody) component that may contribute to the observed spectrum (Mészáros & Rees 2000a; Mészáros et al. 2002; Daigne & Mochkovitch 2002; Rees & Mészáros 2005).”
• FERMI OBSERVATIONS OF GRB 090510: A SHORT–HARD GAMMA-RAY BURST WITH AN ADDITIONAL, HARD POWER-LAW COMPONENT FROM 10 keV TO GeV ENERGIES (2010, background): “This radiation could be from the thermal photosphere made by the powerful relativistic wind (Mészáros et al. 2002; Pe’er et al. 2007), from magnetic reconnection in Poynting-flux dominated outflows (Lyutikov & Blandford 2003), or from nonthermal leptonic emissions formed by internal or external…”
• DISCERNING THE PHYSICAL ORIGINS OF COSMOLOGICAL GAMMA-RAY BURSTS BASED ON MULTIPLE OBSERVATIONAL CRITERIA: THE CASES OF z = 6.7 GRB 080913, z = 8.2 GRB 090423, AND SOME SHORT/HARD GRBs (2009, background): “If abundant pairs are produced, it has been argued that the pair photosphere would effectively screen out the variability time scales smaller than a critical value (Kobayashi et al. 2002; Mészáros et al. 2002).”
• A New Method of Determining the Initial Size and Lorentz Factor of Gamma-Ray Burst Fireballs Using a Thermal Emission Component (2007, methodology): “Depending on the values of the free model parameters (η, L and r0) this radius can be smaller or larger than rs (Mészáros et al. 2002): for η > (<)η∗ ≡ (LσT /4πmpc 3r0) 1/4, rph < (>)rs.”
• Making a Short Gamma-Ray Burst from a Long One: Implications for the Nature of GRB 060614 (2006, background): “Alternatively, a general positive dependence of Ep on Eiso is expected if Ep reflects the thermal peak of the fireball photosphere (Mészáros et al. 2002; Rees & Mészáros 2005; Ryde et al. 2006; Thompson et al. 2006).”
• Gamma-Ray Bursts in the Swift Era (2007, background): “…Ghisellini et al. (2000),Panaitescu & Mészáros (2000), Medvedev (2000), Mészáros & Rees (2000), Spruit et al. (2001), Drenkhahn & Spruit (2002), Mészáros et al. (2002), Zhang & Mészáros (2002c), Dai & Lu (2002a), Pe’er & Waxman (2004a, 2005), Rees & Mészáros (2005), Pe’er et al.…”
• The physics of gamma-ray bursts & relativistic jets (2014, background): “…to explain the prompt γ-ray spectrum, e.g. Thompson (1994); Ghisellini and Celotti (1999); Mészáros and Rees (2000b); Eichler and Levinson (2000); Mészáros et al. (2002); Rees and Mészáros (2005); Pe’er et al. (2006b); Giannios (2006); Giannios and Spruit (2007); Ioka et al. (2007); Pe’er…”
• An Analysis of Gamma-Ray Burst Spectral Break Models (2002, methodology): “[5] of Mészáros et al. 2002 for a more general treatment) and rdec (eq.”
• EVIDENCE OF AN INITIALLY MAGNETICALLY DOMINATED OUTFLOW IN GRB 080916C (2009, background): “The rest of energy is still stored in the form of photons, which escape the system as the fireball becomes transparent at the photosphere radius (Mészáros & Rees 2000; Mészáros et al. 2002).”
• A theory of photospheric emission from relativistic, collimated outflows (2012, background): “Several models predict non-thermal spectral components as a result of kinetic or magnetic energy dissipation above the photosphere (e.g. Mészáros et al. 2002; Zhang & Yan 2011).”
• IDENTIFICATION AND PROPERTIES OF THE PHOTOSPHERIC EMISSION IN GRB090902B (2009, background): “DISCUSSION The presence of a strong photospheric component in GRB spectra has been discussed by several authors (e.g. Goodman 1986; Mészáros et al. 2002; Rees & Mészáros 2005)18.”
• High-resolution calculations of merging neutron stars - III. Gamma-ray bursts (2003, background): “Seen from one viewing angle a burst would appear as a X-ray rich burst (Heise et al. 2001) while from a different angle it would be interpreted as a standard GRB (Salmonson 2000; Ioka & Nakamura 2001; Kobayashi, Ryde & MacFadyen 2002; RamirezRuiz & Lloyd-Ronning 2002; Mészáros et al. 2002).”
• Gamma-Ray Bursts in the Swift Era (2009, background): “…electrons accelerated in the shocks occurring outside it (Mészáros and Rees 2000, Ramirez-Ruiz and Lloyd-Ronning 2002, Spada et al. 2000, Kobayashi et al. 2002, Mészáros et al. 2002, Ramirez-Ruiz 2005, Giannios and Spruit 2007, Pe’er et al. 2006, Ryde and Pe’er 2008, Thompson et al. 2007).”
• The Cooling Behavior of Thermal Pulses in Gamma-Ray Bursts (2004, background): “Aside from the theoretical motivations mentioned above (see, e.g., Mészáros et al. 2002; Daigne & Mochkovitch 2002; Drenkhahn & Spruit 2002; Blinnikov et al. 1999), there are also several authors that have already proposed a thermal origin as an interpretation of the very hardest observed…”
• Global Characteristics of X-Ray Flashes and X-Ray-Rich Gamma-Ray Bursts Observed by HETE-2 (2005, background): “According to Mészáros et al. (2002) and Woosley et al. (2003), X-ray (20–100 keV) photons are produced effectively by the hot cocoon surrounding the GRB jet as it breaks out, and could produce XRF-like events if viewed well off the axis of the jet.”
• THE INTERNAL-COLLISION-INDUCED MAGNETIC RECONNECTION AND TURBULENCE (ICMART) MODEL OF GAMMA-RAY BURSTS (2010, background): “Such a thermal component is predicted bright enough to be usually detectable along with the IS nonthermal emission component (Mészáros and Rees 2000; Mészáros et al. 2002; Pe’er 2008).”
• A COMPREHENSIVE ANALYSIS OF FERMI GAMMA-RAY BURST DATA. I. SPECTRAL COMPONENTS AND THE POSSIBLE PHYSICAL ORIGINS OF LAT/GBM GRBs (2010, background): “…emission from internal shocks (Rees & Mészáros 1994; Kobayashi et al. 1997), the photosphere (Paczýnski 1986; Goodman 1986; Mészáros & Rees 2000; Mészáros et al. 2002; Pe’er 2008), some magnetic dissipation regions (Lyutikov & Blandford 2003; Zhang & Yan 2011), or the external shock…”