Gamma-ray burst long lasting X-ray flaring activity
文献类型：期刊论文
| 作者 | Bernardini, MG1,2; Margutti, R1,3; Chincarini, G1,3; Guidorzi, C4; Mao JR(毛基荣)1,5
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| 刊名 | ASTRONOMY & ASTROPHYSICS
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| 出版日期 | 2011-02 |
| 卷号 | 526 |
| 关键词 | radiation mechanisms: non-thermal gamma-rays: general X-rays: general |
| ISSN号 | 0004-6361 |
| 产权排序 | 第五完成单位 |
| 通讯作者 | Bernardini, MG (reprint author), Osserv Astron Brera, INAF, Via Bianchi 46, I-23807 Merate, LC, Italy. |
| 英文摘要 | Context. One of the most intriguing features revealed by the Swift satellite are flares that are superimposed on the gamma-ray burst (GRB) X-ray light curves. The vast majority of flares occurs before 1000 s, but some of them can be found up to 10(6) s after the main event. Aims. We shed light on late-time (i.e. with peak time t(pk) greater than or similar to 1000 s) flaring activity. We address the morphology and energetic of flares in the window similar to 10(3)-10(6) s to put constraints on the temporal evolution of the flare properties and to identify possible differences in the mechanism producing the early and late-time flaring emission, if any. This requires the complete understanding of the observational biases affecting the detection of X-ray flares superimposed on a fading continuum at t > 1000 s. Methods. We consider all Swift GRBs that exhibit late-time flares. Our sample consists of 36 flares, 14 with redshift measurements. We inherit the strategy of data analysis from Chincarini et al. (2010) in order to make a direct comparison with the early-time flare properties. Results. The morphology of the flare light curve is the same for both early-time and late-time flares, but they differ energetically. The width of late-time flares increases with time similarly to the early-time flares. Simulations confirmed that the increase of the width with time is not owing to the decaying statistics, at least up to 10(4) s. The energy output of late-time flares is one order of magnitude lower than the early-time flare one, and is similar to 1%E-prompt. The evolution of the peak luminosity as well as the distribution of the peak-flux-to-continuum ratio for late-time flares indicate that the flaring emission is decoupled from the underlying continuum, differently from early-time flares/steep decay. A sizable fraction of late-time flares are compatible with afterglow variability. Conclusions. The internal shock origin seems the most promising explanation for flares. However, some differences that emerge between late-and early-time flares suggest that there could be no unique explanation about the nature of late-time flares. |
| WOS标题词 | Science & Technology ; Physical Sciences |
| 学科主题 | Astronomy & Astrophysics |
| 类目[WOS] | Astronomy & Astrophysics |
| 研究领域[WOS] | Astronomy & Astrophysics |
| 关键词[WOS] | LIGHT CURVES ; PROMPT EMISSION ; ENGINE ACTIVITY ; 1ST SURVEY ; FLARES ; SWIFT ; ACCRETION ; AFTERGLOWS ; VARIABILITY ; ENERGETICS |
| 收录类别 | SCI ; EI |
| 原文出处 | http://www.aanda.org/articles/aa/abs/2011/02/aa15703-10/aa15703-10.html |
| 语种 | 英语 |
| WOS记录号 | WOS:000286458400039 |
| 源URL | [http://ir.ynao.ac.cn/handle/114a53/5015]  |
| 专题 | 云南天文台_高能天体物理研究组 云南天文台_中国科学院天体结构与演化重点实验室 |
| 作者单位 | 1.INAF – Osservatorio Astronomico di Brera, via Bianchi 46, 23807 Merate ( LC), Italy 2.ICRANet, p.le della Repubblica 10, 65100 Pescara, Italy 3.University of Milano Bicocca, Physics Dept., P.zza della Scienza 3, Milano 20126, Italy 4.University of Ferrara, Physics Dept., via Saragat 1, 44122 Ferrara, Italy 5.Yunnan Observatory & Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming, Yunnan Province 650011, PR China |
| 推荐引用方式 GB/T 7714 | Bernardini, MG,Margutti, R,Chincarini, G,et al. Gamma-ray burst long lasting X-ray flaring activity[J]. ASTRONOMY & ASTROPHYSICS,2011,526. |
| APA | Bernardini, MG,Margutti, R,Chincarini, G,Guidorzi, C,&Mao JR.(2011).Gamma-ray burst long lasting X-ray flaring activity.ASTRONOMY & ASTROPHYSICS,526. |
| MLA | Bernardini, MG,et al."Gamma-ray burst long lasting X-ray flaring activity".ASTRONOMY & ASTROPHYSICS 526(2011). |
入库方式： OAI收割
来源：云南天文台
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