HETE-2 Observations of the X-Ray Flash XRF 040916
HETE-2 Observations of the X-Ray Flash XRF 040916
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DOI：
10.1093/pasj/59.3.695
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发表时间：
2007-03
影响因子：
2.3
通讯作者：
M. Arimoto;N. Kawai;Motoko Suzuki;R. Sato;N. V. Pazmino;T. Shimokawabe;T. Ishimura;J. Kotoku;A. Yoshida;T. Tamagawa;Y. Shirasaki;M. Matsuoka;Y. Nakagawa;N. Ishikawa;A. Kobayashi;S. Sugita;I. Takahashi;M. Kuwahara;M. Yamauchi;K. Takagishi;I. Hatsukade;J. Atteia;A. Pelangeon;R. Vanderspek;C. Graziani;G. Prigozhin;J. Villasenor;J. Jernigan;G. Crew;K. Hurley;T. Sakamoto;G. Ricker;S. Woosley;N. Butler;A. Levine;J. Doty;T. Donaghy;D. Lamb;E. Fenimore;M. Galassi;M. Boer;J. Dezalay;J. Olive;J. Braga;R. Manchanda;G. Pizzichini
中科院分区：
文献类型：
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作者：
M. Arimoto;N. Kawai;Motoko Suzuki;R. Sato;N. V. Pazmino;T. Shimokawabe;T. Ishimura;J. Kotoku;A. Yoshida;T. Tamagawa;Y. Shirasaki;M. Matsuoka;Y. Nakagawa;N. Ishikawa;A. Kobayashi;S. Sugita;I. Takahashi;M. Kuwahara;M. Yamauchi;K. Takagishi;I. Hatsukade;J. Atteia;A. Pelangeon;R. Vanderspek;C. Graziani;G. Prigozhin;J. Villasenor;J. Jernigan;G. Crew;K. Hurley;T. Sakamoto;G. Ricker;S. Woosley;N. Butler;A. Levine;J. Doty;T. Donaghy;D. Lamb;E. Fenimore;M. Galassi;M. Boer;J. Dezalay;J. Olive;J. Braga;R. Manchanda;G. Pizzichini
2004年9月16日00:03:30 UT，高能瞬变探测器II （HETE-2）上的仪器探测到并定位了一个长x射线闪光。该位置在爆发大约2小时后报告给了GRB坐标网（GCN）。这次爆发由两个峰组成，间隔为？200秒，持续时间约为110秒和60秒。我们分析了广域x射线监测器（WXM）和法国伽玛望远镜（FREGATE）观测到的第1和第2峰的能谱。我们从通量变率和时间尺度的角度讨论了第二个峰的起源。我们发现它很可能是快速排放的一部分，并且可以用长效发动机模型来解释。这一特征与雨燕卫星观测到的爆发的早期余辉阶段探测到的一些明亮的x射线耀斑相似。
A long X-ray flash was detected and localized by instruments aboard the High Energy Transient Explorer II (HETE-2) at 00:03:30 UT on 2004 September 16. The position was reported to the GRB Coordinates Network (GCN) approximately 2 hours after the burst. This burst consisted of two peaks separated by ? 200 s, with durations of about 110 s and 60 s. We analyzed the energy spectra of the 1st and 2nd peaks observed with the Wide Field X-Ray Monitor (WXM) and the French Gamma Telescope (FREGATE). We discuss the origin of the 2nd peak in terms of the flux variabilities and timescales. We find that it is most likely to be part of prompt emission, and is explained by a long-acting engine model. This feature is similar to some bright X-ray flares detected in the early afterglow phase of bursts observed by the Swift satellite.