Chincarini 2010 X射线耀发的一些特性

主要内容:
分析了很多XRFs，得到了很多数据，以及如下的结论：
1. 宽度越宽，能量越低， w～E^-1/2.可以理解，原因是越宽的越晚，自然能量比较低。
2. 耀发的形状比较不对称，t_rise/t_decay~0.5；
3. 对同一个暴，多个耀发的时标是随时间变长的，但2中的比例不变；
4. 时标w～0.2t_peak（这个值应该比较有价值）;
5. 峰值光度随时间降低（这个太明显了）；
6. 各向同性能1e51erg，比暴本身低，谱比暴本身软（也是可预期的）；
7. 多个flares也是越来越软（不奇怪）。

精彩摘抄:

他们的拟合过程

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Title:		Unveiling the origin of X-ray flares in gamma-ray bursts
Authors:		Chincarini, G.; Mao, J.; Margutti, R.; Bernardini, M. G.; Guidorzi, C.; Pasotti, F.; Giannios, D.; Valle, M. Della; Moretti, A.; Romano, P.; D'Avanzo, P.; Cusumano, G.; Giommi, P.
Affiliation:		AA(INAF - Osservatorio Astronomico di Brera, via Bianchi 46, I-23807 Merate (LC), Italy; Physics Department, University of Milano Bicocca, Piazza della Scienza 3, Milano 20126, Italy), ...
Publication:		Monthly Notices of the Royal Astronomical Society, Volume 406, Issue 4, pp. 2113-2148. (MNRAS Homepage)
Publication Date:		08/2010
Origin:		WILEY
MNRAS Keywords:		radiation mechanisms: non-thermal, gamma-ray burst: general, X-rays: bursts
Abstract Copyright:		(c) Journal compilation © 2010 RAS
DOI:		10.1111/j.1365-2966.2010.17037.x
Bibliographic Code:		2010MNRAS.406.2113C

Abstract

ABSTRACT We present an updated catalogue of 113 X-ray flares detected by Swift in the ~33 per cent of the X-ray afterglows of gamma-ray burst (GRB). 43 flares have a measured redshift. For the first time the analysis is performed in four different X-ray energy bands, allowing us to constrain the evolution of the flare temporal properties with energy. We find that flares are narrower at higher energies: their width follows a power-law relation w ~ E^-0.5 reminiscent of the prompt emission. Flares are asymmetric structures, with a decay time which is twice the rise time on average. Both time-scales linearly evolve with time, giving rise to a constant rise-to-decay ratio: this implies that both time-scales are stretched by the same factor. As a consequence, the flare width linearly evolves with time to larger values: this is a key point that clearly distinguishes the flare from the GRB prompt emission. The flare 0.3-10keV peak luminosity decreases with time, following a power-law behaviour with large scatter: L_pk ~ t^-2.7+/-0.5_pk. When multiple flares are present, a global softening trend is established: each flare is on average softer than the previous one. The 0.3-10 keV isotropic energy distribution is a lognormal peaked at 10⁵¹erg, with a possible excess at low energies. The flare average spectral energy distribution is found to be a power law with spectral energy index β ~ 1.1. These results confirmed that the flares are tightly linked to the prompt emission. However, after considering various models we conclude that no model is currently able to account for the entire set of observations.

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