PHENOMENOLOGY OF REVERSE-SHOCK EMISSION IN THE OPTICAL AFTERGLOWS OF GAMMA-RAY BURSTS
PHENOMENOLOGY OF REVERSE-SHOCK EMISSION IN THE OPTICAL AFTERGLOWS OF GAMMA-RAY BURSTS
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DOI：
10.1088/0004-637x/785/2/84
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发表时间：
2014-04-20
影响因子：
4.9
通讯作者：
Gomboc, A.
中科院分区：
文献类型：
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作者：
Japelj, J.;Kopac, D.;Gomboc, A.
我们使用118个伽玛射线暴（GRB）余辉的母样本，已知红移和宿主星系消光，以区分具有和不具有主导逆激波（RS）发射特征的余辉，并确定哪些物理条件导致突出的逆激波发射。我们确定了具有反向激波特征的10grb: 990123、021004、021211、060908、061126、080319B、081007、090102、090424和130427A。通过对它们的光学余辉进行反向和正激解析光曲线建模，并使用蒙特卡罗模拟，我们估计了描述喷射物和环爆介质的物理量的参数空间。我们发现物理性质覆盖了一个广泛的参数空间，并且似乎不围绕任何优先值聚集。通过比较非rs主导型GRBs大样本的静帧光学、x射线和高能特性，我们发现早期（10 ks）的GRBs存在。我们发现，具有可识别的逆激波分量的grb具有高磁化参数r -B = epsilon(B,r)/epsilon(B,f)，类似于2-10(4)。我们的结果与伽玛暴的轻度磁化重子射流模型一致。
We use a parent sample of 118 gamma-ray burst (GRB) afterglows, with known redshift and host galaxy extinction, to separate afterglows with and without signatures of dominant reverse-shock (RS) emission and to determine which physical conditions lead to a prominent reverse-shock emission. We identify 10GRBs with reverse-shock signatures: 990123, 021004, 021211, 060908, 061126, 080319B, 081007, 090102, 090424, and 130427A. By modeling their optical afterglows with reverse-and forward-shock analytic light curves and using Monte Carlo simulations, we estimate the parameter space of the physical quantities describing the ejecta and circumburst medium. We find that physical properties cover a wide parameter space and do not seem to cluster around any preferential values. Comparing the rest-frame optical, X-ray, and high-energy properties of the larger sample of non-RS-dominated GRBs, we show that the early-time ( 10 ks). We find that GRBs with an identifiable reverse-shock component show a high magnetization parameter R-B = epsilon(B,r)/epsilon(B,f) similar to 2-10(4). Our results are in agreement with the mildly magnetized baryonic jet model of GRBs.