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首页> 外文期刊>The Astrophysical journal >WIND-INTERACTION MODELS FOR THE EARLY AFTERGLOWS OF GAMMA-RAY BURSTS: THE CASE OF GRB 021004
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WIND-INTERACTION MODELS FOR THE EARLY AFTERGLOWS OF GAMMA-RAY BURSTS: THE CASE OF GRB 021004

机译：伽玛射线爆发后早期的风相互作用模型：以GRB 021004为例

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Wind-interaction models for gamma-ray burst (GRB) afterglows predict that the optical emission from the reverse shock drops below that from the forward shock within hundreds of seconds of the burst. The typical frequency v_m of the synchrotron emission from the forward shock passes through the optical band typically on a timescale of minutes to hours. Before the passage of v_m, the optical flux evolves as t~(-1/4), and after the passage, the decay steepens to t~(-(3p-2)/4), where p is the exponent for the assumed power-law energy distribution of nonthermal electrons and is typically ～2. The steepening in the slope of temporal decay should be readily identifiable in the early afterglow light curves. We propose that such a steepening was observed in the R-band light curve of GRB 021004 around day 0.1. Available data at several radio frequencies are consistent with this interpretation, as are the X-ray observations around day 1. The early evolution of GRB 021004 contrasts with that of GRB 990123, which can be described by emission from interaction with a constant density medium.
机译：伽马射线爆发（GRB）余辉的风相互作用模型预测，在爆发的数百秒内，来自反向冲击的光发射将低于来自向前冲击的光发射。来自前向冲击的同步加速器发射的典型频率v_m通常在几分钟到几小时的时间内通过光学波段。在v_m通过之前，光通量演化为t〜（-1/4），而在通过之后，衰减变陡至t〜（-（3p-2）/ 4），其中p是假定的指数非热电子的幂律能量分布通常为〜2。在早期余辉光曲线中应易于识别出时间衰减斜率的陡峭。我们建议在第0.1天左右的GRB 021004的R波段光曲线中观察到这种变陡。与第1天前后的X射线观察结果相同，几个无线电频率处的可用数据也与这种解释一致。GRB 021004的早期演变与GRB 990123的早期演变形成对比，这可以通过与恒定密度介质相互作用的发射来描述。

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