Burgess, J. Michael 2011 GRB 090820A暴本身的辐射机制

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Title:		Constraints on the Synchrotron Shock Model for the Fermi GRB 090820A Observed by Gamma-Ray Burst Monitor
Authors:		Burgess, J. Michael; Preece, Robert D.; Baring, Matthew G.; Briggs, Michael S.; Hodge, Colleen
Affiliation:		AA(Department of Physics, University of Alabama in Huntsville,
Publication:		The Astrophysical Journal, Volume 741, Issue 1, article id. 24 (2011). (ApJ Homepage)
Publication Date:		11/2011
Origin:		IOP
Astronomy Keywords:		acceleration of particles, gamma-ray burst: individual: GRB 090820A, gamma rays: stars, methods: data analysis, radiation mechanisms: non-thermal, radiation mechanisms: thermal
DOI:		10.1088/0004-637X/741/1/24
Bibliographic Code:		2011ApJ...741...24B

Abstract

Discerning the radiative dissipation mechanism for prompt emission in gamma-ray bursts (GRBs) requires detailed spectroscopic modeling that straddles the νF _ν peak in the 100 keV-1 MeV range. Historically, empirical fits such as the popular Band function have been employed with considerable success in interpreting the observations. While extrapolations of the Band parameters can provide some physical insight into the emission mechanisms responsible for GRBs, these inferences do not provide a unique way of discerning between models. By fitting physical models directly, this degeneracy can be broken, eliminating the need for empirical functions; our analysis here offers a first step in this direction. One of the oldest, and leading, theoretical ideas for the production of the prompt signal is the synchrotron shock model. Here we explore the applicability of this model to a bright Fermi gamma-ray burst monitor (GBM) burst with a simple temporal structure, GRB 090820A. Our investigation implements, for the first time, thermal and non-thermal synchrotron emissivities in the RMFIT forward-folding spectral analysis software often used in GBM burst studies. We find that these synchrotron emissivities, together with a blackbody shape, provide at least as good a match to the data as the Band GRB spectral fitting function. This success is achieved in both time-integrated and time-resolved spectral fits.

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