CONSTRAINING GAMMA-RAY BURST EMISSION PHYSICS WITH EXTENSIVE EARLY-TIME, MULTIBAND FOLLOW-UP
CONSTRAINING GAMMA-RAY BURST EMISSION PHYSICS WITH EXTENSIVE EARLY-TIME, MULTIBAND FOLLOW-UP
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DOI：
10.1088/0004-637x/743/2/154
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发表时间：
2011-07
期刊：
影响因子：
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通讯作者：
A. Cucchiara;A. Cucchiara;S. Cenko;J. Bloom;A. Melandri;A. Melandri;A. Morgan;S. Kobayashi;Robert J. Smith;D. Perley;Weidong Li;J. Hora;R. D. Silva;J. Prochaska;Peter Milne;N. Butler;B. Cobb;G. Worseck;C. Mundell;I. Steele;A. Filippenko;Michele Fumagalli;C. Klein;A. Stephens;A. Bluck;R. Mason
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文献类型：
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作者：
A. Cucchiara;A. Cucchiara;S. Cenko;J. Bloom;A. Melandri;A. Melandri;A. Morgan;S. Kobayashi;Robert J. Smith;D. Perley;Weidong Li;J. Hora;R. D. Silva;J. Prochaska;Peter Milne;N. Butler;B. Cobb;G. Worseck;C. Mundell;I. Steele;A. Filippenko;Michele Fumagalli;C. Klein;A. Stephens;A. Bluck;R. Mason
了解造成伽马射线暴(伽马射线暴)的发射过程的来源和多样性仍然是一项紧迫的挑战。虽然即时和同期的全色观测有可能检验内部-外部激波模型的预测，但只对少数几个伽玛暴进行了广泛的多波段成像。我们为两个SWIFT事件GRB 110205A和GRB 110213A提供了丰富的早期多波段数据集。前者显示了从瞬发阶段开始的光发射，然后是爆发后通量急剧上升，直到∼1000时S(t−α，α=−为6.13±0.75)。我们在反向激波情形下讨论了这一特征，并将下面的单次幂函数衰变解释为正激波占优势。安装在利物浦望远镜上的RINGO2仪器获得的偏振测量也为发射出的喷射物的性质提供了线索。相反，后一次事件显示了一条非常特殊的光学到近红外线的光曲线，有两个非色差峰。在这种情况下，虽然第一个峰值可能是由于余辉的开始，但我们解释第二个峰值是由新注入的物质产生的，这意味着中央引擎的后期活动。
Understanding the origin and diversity of emission processes responsible for gamma-ray bursts (GRBs) remains a pressing challenge. While prompt and contemporaneous panchromatic observations have the potential to test predictions of the internal–external shock model, extensive multiband imaging has been conducted for only a few GRBs. We present rich, early-time, multiband data sets for two Swift events, GRB 110205A and GRB 110213A. The former shows optical emission since the early stages of the prompt phase, followed by the steep rising in flux up to ∼1000 s after the burst (t−α with α = −6.13 ± 0.75). We discuss this feature in the context of the reverse-shock scenario and interpret the following single power-law decay as being forward-shock dominated. Polarization measurements, obtained with the RINGO2 instrument mounted on the Liverpool Telescope, also provide hints on the nature of the emitting ejecta. The latter event, instead, displays a very peculiar optical to near-infrared light curve, with two achromatic peaks. In this case, while the first peak is probably due to the onset of the afterglow, we interpret the second peak to be produced by newly injected material, signifying a late-time activity of the central engine.