An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog

被引：17

作者：

Cai, Ce ^{[1
,2
]}

Xiong, Shao-Lin ^{[1
]}

Lin, Lin ^{[3
]}

Li, Cheng-Kui ^{[1
]}

Zhang, Shuang-Nan ^{[1
,2
]}

Xue, Wang-Chen ^{[1
,2
]}

Tuo, You-Li ^{[1
]}

Li, Xiao-Bo ^{[1
]}

Ge, Ming-Yu ^{[1
]}

Zhao, Hai-Sheng ^{[1
]}

Song, Li-Ming ^{[1
,2
]}

Lu, Fang-Jun ^{[1
,2
]}

Zhang, Shu ^{[1
]}

Li, Qing-Xin ^{[3
]}

Xiao, Shuo ^{[1
,2
]}

Guo, Zhi-Wei ^{[1
,4
]}

Xie, Sheng-Lun ^{[1
,5
]}

Zhang, Yan-Qiu ^{[1
,2
]}

Yi, Qi-Bin ^{[1
,6
]}

Zhao, Yi ^{[1
,3
]}

Zhang, Zhen ^{[1
]}

Liu, Jia-Cong ^{[1
,2
]}

Zheng, Chao ^{[1
,2
]}

Wang, Ping ^{[1
]}

机构：

[1] Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, 19B Yuquan Rd, Beijing 100049, Peoples R China

[2] Univ Chinese Acad Sci, Chinese Acad Sci, Beijing 100049, Peoples R China

[3] Beijing Normal Univ, Dept Astron, Beijing 100088, Peoples R China

[4] Hebei Univ, Coll Phys Sci Technol, 180 Wusi Dong Rd, Baoding City 071002, Hebei, Peoples R China

[5] Cent China Normal Univ, Sch Phys Sci & Technol, Wuhan 430097, Peoples R China

[6] Xiangtan Univ, Sch Phys & Optoelect, Xiangtan 411105, Hunan, Peoples R China

来源：

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES | 2022年 / 260卷 / 02期

基金：

中国国家自然科学基金; 国家重点研发计划;

关键词：

X-RAY PULSAR; MAGNETAR; FLARE; EMISSION; VIEW;

D O I：

10.3847/1538-4365/ac67e4

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Since 2020 April 28, Insight-HXMT has implemented a dedicated observation on the magnetar SGR J1935+2154. Thanks to the wide energy band (1-250 keV) and high sensitivity of Insight-HXMT, we obtained 75 bursts from SGR J1935+2154 during a month-long activity episode after the emission of FRB 200428. Here we report the detailed time-integrated spectral analysis of these bursts and the statistical distribution of the spectral parameters. We find that for similar to 15% (11/75) of SGR J1935+2154 bursts, the CPL model is preferred, and most of them occurred in the later part of this active epoch. In the cumulative fluence distribution, we find that the fluence of bursts in our sample is about an order of magnitude weaker than that of Fermi/GBM, but it follows the same power-law distribution. Finally, we find a burst with similar peak energy to the time-integrated spectrum of the X-ray burst associated with FRB 200428 (FRB 200428-Associated Burst), but the low energy index is harder.

引用

页数：14

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