Mimica 2010 MHD数值模拟余辉辐射

主要内容:
考虑磁化的外流体，磁化系数sigma

精彩摘抄:


文章信息:

· Find Similar Abstracts (with default settings below)

· Electronic Refereed Journal Article (HTML)

· Full Refereed Journal Article (PDF/Postscript)

· arXiv e-print (arXiv:1004.2720)

· References in the article

· Citations to the Article (1) (Citation History)

· Refereed Citations to the Article

· Also-Read Articles (Reads History)

·

· Translate This Page

Title:		Multiwavelength afterglow light curves from magnetized gamma-ray burst flows
Authors:		Mimica, P.; Giannios, D.; Aloy, M. A.
Affiliation:		AA(Departamento de Astronomía y Astrofísica, Universidad de Valencia, 46100 Burjassot, Spain), AB(Department of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, NJ 08544, USA), AC(Departamento de Astronomía y Astrofísica, Universidad de Valencia, 46100 Burjassot, Spain)
Publication:		Monthly Notices of the Royal Astronomical Society, Online Early (MNRAS Homepage)
Publication Date:		06/2010
Origin:		WILEY
MNRAS Keywords:		hydrodynamics, MHD, radiation mechanisms: non-thermal, radiative transfer, shock waves, gamma-ray burst: general
Abstract Copyright:		(c) Journal compilation © 2010 RAS
DOI:		10.1111/j.1365-2966.2010.17071.x
Bibliographic Code:		2010MNRAS.tmp.1005M

Abstract

ABSTRACT We use high-resolution relativistic magnetohydrodynamics simulations coupled with a radiative transfer code to compute multiwavelength afterglow light curves of magnetized ejecta of gamma-ray bursts interacting with a uniform circumburst medium. The aim of our study is to determine how the magnetization of the ejecta at large distance from the central engine influences the afterglow emission, and to assess whether observations can be reliably used to infer the strength of the magnetic field. We find that, for typical parameters of the ejecta, the emission from the reverse shock peaks for magnetization σ₀ ~ 0.01-0.1 of the flow, and that it is greatly suppressed for higher σ₀. The emission from the forward shock shows an achromatic break shortly after the end of the burst marking the onset of the self-similar evolution of the blast wave. Fitting the early afterglow of GRBs 990123 and 090102 with our numerical models we infer respective magnetizations of σ₀ ~ 0.01 and σ₀ ~ 0.1 for these bursts. We argue that the lack of observed reverse shock emission from the majority of the bursts can be understood if σ₀ >~ 0.1, since we obtain that the luminosity of the reverse shock decreases significantly for σ₀ ~ 1. For ejecta with σ₀ >~ 0.1 our models predict that there is sufficient energy left in the magnetic field, at least during an interval of ~ 10 times the burst duration, to produce a substantial emission if the magnetic energy can be dissipated (for instance, due to resistive effects) and radiated away.

---

Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)