Willingale 2009 对伽马暴脉冲的上升和下降阶段的统计

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精彩摘抄:

L_f是T_f时候的光度, T_f是pulse的峰值所出现的时间。 L_f随T_f减小说明越晚脉冲越弱。

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Title:		The spectral-temporal properties of the prompt pulses and rapid decay phase of gamma-ray bursts
Authors:		Willingale, R.; Genet, F.; Granot, J.; O'Brien, P. T.
Affiliation:		AA(Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH), AB(Center for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB; Racah Institute of Physics, Hebrew University of Jerusalem, Israel), AC(Center for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB), AD(Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH)
Publication:		Monthly Notices of the Royal Astronomical Society, Volume 403, Issue 3, pp. 1296-1316. (MNRAS Homepage)
Publication Date:		04/2010
Origin:		WILEY
MNRAS Keywords:		radiation mechanisms: non-thermal, ISM: jets and outflows, gamma-rays: bursts
DOI:		10.1111/j.1365-2966.2009.16187.x
Bibliographic Code:		2010MNRAS.403.1296W

Abstract

The prompt emission from gamma-ray burst is the brightest electromagnetic emission known, yet its origin is not understood. The flux density of individual prompt pulses of a GRB can be represented by an analytical expression derived assuming the emission is from a thin, ultrarelativistically expanding, uniform, spherical shell over a finite range of radii. We present the results of fitting this analytical expression to the light curves from the four standard Swift Burst Alert Telescope energy bands and two standard Swift X-ray Telescope energy bands of 12 bursts. The expression includes the high latitude emission (HLE) component and the fits provide a rigorous demonstration that the HLE can explain the rapid decay phase of the prompt emission. The model also accommodates some aspects of energy-dependent lag and energy-dependent pulse width, but there are features in the data which are not well represented. Some pulses have a hard, narrow peak which is not well fitted or a rise and decay which are faster than expected using the standard indices derived assuming synchrotron emission from internal shocks, although it might be possible to accommodate these features using a different emission mechanism within the same overall framework. The luminosity of pulses is correlated with the peak energy of the pulse spectrum, L_f ~ [E_peak(1 + z)]^1.8, and anticorrelated with the time since ejection of the pulse, L_f ~ [T_f/(1 + z)]^-2.0.

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