The expected thermal precursors of gamma-ray bursts in the internal shock model

By F. Daigne, R. M. S. d'AstrophysiqueDAPNIACEA, Saclay, France., I. D. Paris. 2002

154 citations recorded by the source corpus.

The prompt emission of gamma-ray bursts probably comes from a highly relativistic wind which converts part of its kinetic energy into radiation via the formation of shocks within the wind itself. Such ‘internal shocks’ can occur if the wind is generated with a highly non-uniform distribution of the Lorentz factor. We estimate the expected photospheric emission of such a relativistic wind when it becomes transparent. We compare this thermal emission (temporal profile + spectrum) with the non-thermal emission produced by the internal shocks. In most cases, we predict a rather bright thermal emission that should already have been detected. This favours acceleration mechanisms for the wind where the initial energy input is under magnetic rather than thermal form. Such scenarios can produce thermal X-ray precursors comparable to those observed by Ginga and WATCH/GRANAT.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/febcb5d0eb39a360408229b867e1380ae3234dde

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In Astronomy and Astrophysics

1. Bing Zhang
2. Pawan Kumar
3. F. Ryde
4. E. Nakar
5. A. Pe’er
6. E. Liang
7. Binbin Zhang
8. D. Giannios

In Nuclear and High Energy Physics

1. Bing Zhang
2. Pawan Kumar
3. D. Giannios
4. F. Ryde
5. G. Ghisellini
6. E. Liang
7. T. Piran
8. A. Pe’er

Citations in the corpus

• EVIDENCE OF AN INITIALLY MAGNETICALLY DOMINATED OUTFLOW IN GRB 080916C (2009, background): “It has been suggested (Zhang & Mészáros 2002; Daigne & Mochkovitch 2002) that the photosphere thermal component can be much dimmer if the outflow is Poynting flux dominated.”
• Collisional mechanism for gamma‐ray burst emission (2009, background): “It was argued thatthe absence of the photospheric emission component would implythat the jet is magnetically dominated and cold, with negligibleinitial thermal energy (e.g. Daigne & Mochkovitch 2002; Zhang & Pe’er 2009).”
• DETECTION OF A THERMAL SPECTRAL COMPONENT IN THE PROMPT EMISSION OF GRB 100724B (2010, background): “Daigne and Mochkovitch (2002) pointed out that in the standard fireball model, the photospheric component can easily be dominant in the spectrum if the efficiency fNT of the mechanism responsible for the non-thermal emission is only moderate (fNT ∼ 40%).”
• IDENTIFICATION AND PROPERTIES OF THE PHOTOSPHERIC EMISSION IN GRB090902B (2009, background): “Here 18 see also e.g. Paczynski (1986); Mészáros & Rees (2000); Lyutikov & Usov (2000); Daigne & Mochkovitch (2002); 4 we have identified a strong photospheric component in GRB090902B, which is modelled by a multicolor blackbody.”
• The physics of gamma-ray bursts & relativistic jets (2014, background): “…2009c,a; Liang et al., 2010) — and therefore η >∼ 10 2 — the non-detection of a thermal component would imply that the GRB jet was launched with a relatively small radiation component thereby strengthening the case for a Poynting outflow (e.g. Daigne and Mochkovitch, 2002; Zhang and Pe’er, 2009).”
• THE OBSERVABLE SIGNATURES OF GRB COCOONS (2016, background): “The dynamics of relativistic fireballs has been discuss by many authors (see e.g. Goodman 1986; Shemi & Piran 1990; Meszaros et al. 1993; Piran et al. 1993; Grimsrud & Wasserman 1998; Daigne & Mochkovitch 2002; Nakar et al. 2005)6.”
• Prompt emission spectra from the photosphere of a GRB (2006, background): “In that case, a thermal peak should be systematically observed in the prompt GRB spectra, which is not the case (Daigne & Mochkovitch 2002).”
• A COMPREHENSIVE ANALYSIS OF FERMI GAMMA-RAY BURST DATA. I. SPECTRAL COMPONENTS AND THE POSSIBLE PHYSICAL ORIGINS OF LAT/GBM GRBs (2010, background): “In the fireball shock model, such a quasi-blackbody component is expected to be associated with the non-thermal emission components (Mészáros & Rees 2000; Mészáros et al. 2002; Daigne & Mochkovitch 2002; Pe’er et al. 2006).”
• Reconciling observed gamma-ray burst prompt spectra with synchrotron radiation? (2010, background): “One possibility in such cases would be the appear- ance of a quasi-thermal component of photospheric origin (Mészáros & Rees 2000; Daigne & Mochkovitch 2002; Pe’er 2008; Beloborodov 2010; Pe’er et al. 2010).”
• Extremely hard GRB spectra prune down the forest of emission models (2002, methodology): “In this scenario we have two options: we can relate the initial phase to a single fireball, in the process of becoming optically thin, or – following Daigne & Mochkovitch (2002) – to an ensemble ofN shells, each becoming optically thin at approximately the same distance.”
• Relativistic Magnetohydrodynamics with Application to Gamma-Ray Burst Outflows. I. Theory and Semianalytic Trans-Alfvénic Solutions (2003, background): “…been realized that energy deposition by annihilating neutrinos, which had been one of the main proposed heating mechanisms, would typically be inefficient (e.g., 1 Di Matteo, Perna, & Narayan 2002), and it was, furthermore, argued (Daigne & Mochkovitch 2002) that only a small fraction (.”
• A New Method of Determining the Initial Size and Lorentz Factor of Gamma-Ray Burst Fireballs Using a Thermal Emission Component (2007, methodology): “In the case rph > rs, the photospheric radius is given by rph = (LσT /8πη 3mpc 3) (Mészáros et al. 2002; Daigne & Mochkovitch 2002; Broderick 2005).”
• The Cooling Behavior of Thermal Pulses in Gamma-Ray Bursts (2004, methodology): “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…”
• 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).”
• Is Thermal Emission in Gamma-Ray Bursts Ubiquitous? (2005, background): “A strong photospheric emission at γ−ray wave lengths is predicted in most GRB scenarios , such as in kinetic models (Mészáros, & Rees 2000; Daigne & Mochkovitch 2002), in MHD models (Drenkhahn & Spruit 2002), as well as in Poynting flux models (Lyutikov & – 5 – Usov 2000).”
• Short-hard gamma-ray bursts (2007, background): “…fireball remains optically thick until almost all the the energy is converted into bulk motion kinetic energy (Shemi & Piran, 1990; Piran, Shemi & Narayan, 1993; Mészáros, Laguna & Rees, 1993; Grimsrud & Wasserman, 1998; Daigne & Mochkovitch, 2002b; Nakar, Piran & Sari, 2005; Li & Sari, 2006).”