| Unveiling the origin of X-ray flares in gamma-ray bursts | |
Chincarini, G1,2; Mao JR(毛基荣)1,3,4 ; Margutti, R1,2; Bernardini, MG1,5; Guidorzi, C6; Pasotti, F1; Giannios, D7; Della Valle, M5,8; Moretti, A1; Romano, P9; D'Avanzo, P1; Cusumano, G9; Giommi, P10,11; Chincarini, G (reprint author), INAF Osservatorio Astron Brera, Via Bianchi 46, I-23807 Merate, LC, Italy.
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| 发表期刊 | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
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| 2010-08-21 | |
| 卷号 | 406期号:4页码:2113-2148 |
| DOI | 10.1111/j.1365-2966.2010.17037.x |
| 产权排序 | 第3完成单位 |
| 收录类别 | SCI |
| 关键词 | Radiation Mechanisms: Non-thermal Gamma-ray Burst: General X-rays: Bursts |
| 摘要 | We present an updated catalogue of 113 X-ray flares detected by Swift in the similar to 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 proportional to 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 0.3-10 keV peak luminosity decreases with time, following a power-law behaviour with large scatter: L(pk) proportional to 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 1051 erg, with a possible excess at low energies. The flare average spectral energy distribution is found to be a power law with spectral energy index beta similar to 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. |
| 项目资助者 | ASI [SWIFT I/011/07/0] ; Ministry of University and Research of Italy ; MAE ; University of Milano Bicocca (Italy) |
| 语种 | 英语 |
| 学科领域 | Astronomy & Astrophysics |
| 文章类型 | Article |
| ISSN | 0035-8711 |
| URL | 查看原文 |
| WOS记录号 | WOS:000280672600001 |
| WOS研究方向 | Astronomy & Astrophysics |
| WOS类目 | Astronomy & Astrophysics |
| 关键词[WOS] | INTERNAL SHOCKS ; ENGINE ACTIVITY ; LIGHT CURVES ; RELATIVISTIC TURBULENCE ; TEMPORAL PROPERTIES ; SPECTRAL PROPERTIES ; BATSE OBSERVATIONS ; OPTICAL-EMISSION ; REVERSE SHOCK ; 1ST SURVEY |
| 引用统计 | |
| 文献类型 | 期刊论文 |
| 条目标识符 | http://ir.ynao.ac.cn/handle/114a53/4994 |
| 专题 | 高能天体物理研究组 中国科学院天体结构与演化重点实验室 |
| 通讯作者 | Chincarini, G (reprint author), INAF Osservatorio Astron Brera, Via Bianchi 46, I-23807 Merate, LC, Italy. |
| 作者单位 | 1.INAF – Osservatorio Astronomico di Brera, via Bianchi 46, I-23807 Merate (LC), Italy 2.Physics Department, University of Milano Bicocca, Piazza della Scienza 3, Milano 20126, Italy 3.Yunnan Observatory, Chinese Academy of Sciences, Kunming, Yunnan Province 650011, China 4.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming, Yunnan Province 650011, China 5.CRANet, p.le della Repubblica 10, I-65100 Pescara, Italy 6.Physics Department, University of Ferrara, via Saragat 1, I-44122 Ferrara, Italy 7.Department of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, NJ 08544, USA 8.INAF – Osservatorio di Capodimonte, Salita Moiariello 16, I-80131 Napoli, Italy 9.INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, Via La Malfa 153, I-90146 Palermo, Italy 10.ASI Science Data Centre (ASDC), via G. Galilei, I-00044 Frascati (RM), Italy 11.ASI – Unitá Osservazione dellUniverso, viale Liegi 26, I-00198 Roma, Italy |
| 推荐引用方式 GB/T 7714 | Chincarini, G,Mao JR,Margutti, R,et al. Unveiling the origin of X-ray flares in gamma-ray bursts[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2010,406(4):2113-2148. |
| APA | Chincarini, G.,Mao JR.,Margutti, R.,Bernardini, MG.,Guidorzi, C.,...&Chincarini, G .(2010).Unveiling the origin of X-ray flares in gamma-ray bursts.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,406(4),2113-2148. |
| MLA | Chincarini, G,et al."Unveiling the origin of X-ray flares in gamma-ray bursts".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 406.4(2010):2113-2148. |
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