Margutti, R. 2010 x射线耀发和伽马暴都满足L_P-t_lag的关系

主要内容:
都满足L～1/T_lag，说明暴和XRFs同源。
还做了很多别的量的统计。

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Title:		Lag-luminosity relation in γ-ray burst X-ray flares: a direct link to the prompt emission
Authors:		Margutti, R.; Guidorzi, C.; Chincarini, G.; Bernardini, M. G.; Genet, F.; Mao, J.; Pasotti, F.
Affiliation:		AA(INAF Osservatorio Astronomico di Brera, via Bianchi 46, Merate 23807, Italy; Physics Department, University of Milano Bicocca, Piazza della Scienza 3, Milano 20126, Italy), AB(Physics Department, University of Ferrara, via Saragat 1, I-44122 Ferarra, Italy), AC(INAF Osservatorio Astronomico di Brera, via Bianchi 46, Merate 23807, Italy; Physics Department, University of Milano Bicocca, Piazza della Scienza 3, Milano 20126, Italy), AD(INAF Osservatorio Astronomico di Brera, via Bianchi 46, Merate 23807, Italy), AE(Racah Institute of Physics, Hebrew University of Jerusalem, Israel), AF(INAF Osservatorio Astronomico di Brera, via Bianchi 46, Merate 23807, Italy), AG(INAF Osservatorio Astronomico di Brera, via Bianchi 46, Merate 23807, Italy)
Publication:		Monthly Notices of the Royal Astronomical Society, Volume 406, Issue 4, pp. 2149-2167. (MNRAS Homepage)
Publication Date:		08/2010
Origin:		WILEY
MNRAS Keywords:		radiation mechanisms: non-thermal, gamma-ray burst: general
Abstract Copyright:		(c) Journal compilation © 2010 RAS
DOI:		10.1111/j.1365-2966.2010.16824.x
Bibliographic Code:		2010MNRAS.406.2149M

Abstract

ABSTRACT The temporal and spectral analysis of nine bright X-ray flares out of a sample of 113 flares observed by Swift reveals that the flare phenomenology is strictly analogous to the prompt γ-ray emission: high-energy flare profiles rise faster, decay faster and peak before the low-energy emission. However, flares and prompt pulses differ in one crucial aspect: flares evolve with time. As time proceeds, flares become wider, with larger peak lag, lower luminosities and softer emission. The flare spectral peak energy E_p,i evolves to lower values following an exponential decay which tracks the decay of the flare flux. The two flares with best statistics show higher than expected isotropic energy E_iso and peak luminosity L_p,iso when compared to the E_p,i-E_iso and E_p,i-L_iso prompt correlations. E_p,i is found to correlate with L_iso within single flares, giving rise to a time-resolved E_p,i(t)-L_iso(t). Like prompt pulses, flares define a lag-luminosity relation: L^0.3-10keV_p,iso ~ t^-0.95+/-0.23_lag. The lag-luminosity is proven to be a fundamental law extending ~5 decades in time and ~5 decades in energy. Moreover, this is direct evidence that γ-ray burst (GRB) X-ray flares and prompt γ-ray pulses are produced by the same mechanism. Finally we establish a flare-afterglow morphology connection: flares are preferentially detected superimposed to one-break or canonical X-ray afterglows.

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Title:		Lag-luminosity relation in gamma-ray burst X-ray flares
Authors:		Margutti, R.
Publication:		eprint arXiv:1006.4103
Publication Date:		06/2010
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		To appear in: "Deciphering the ancient universe with GRBs", Kyoto 2010, conference proceeding
Bibliographic Code:		2010arXiv1006.4103M

Abstract

In strict analogy to prompt pulses, X-ray flares observed by Swift-XRT in long Gamma-Ray Bursts define a lag-luminosity relation: L_p,iso \propto t_lag^{-0.95+/-0.23}. The lag-luminosity is proven to be a fundamental law extending 5 decades in time and 5 in energy. This is direct evidence that GRB X-ray flares and prompt gamma-ray pulses are produced by the same mechanism.

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