Insights into the X-Ray Burst Pulse Morphology from SGR J1935+2154

被引：0

作者：

Yang, Jiao-Jiao ^{[1
,2
]}

Xiao, Shuo ^{[1
,2
]}

Wang, Yue ^{[3
]}

Xiong, Shao-Lin ^{[3
]}

Lin, Lin ^{[4
]}

Jiang, Zheng-Huo ^{[1
,2
]}

Liao, Tong-Lei ^{[1
,2
]}

Li, Xiao-Bo ^{[3
]}

Li, Cheng-Kui ^{[3
]}

Yi, Shu-Xu ^{[3
]}

Zhang, Zhen ^{[3
]}

Zhang, Shuang-Nan ^{[3
,5
]}

机构：

[1] Guizhou Normal Univ, Sch Phys & Elect Sci, Guiyang 550001, Peoples R China

[2] Guizhou Normal Univ, Guizhou Prov Key Lab Radio Astron & Data Proc, Guiyang 550001, Peoples R China

[3] Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, Beijing 100049, Peoples R China

[4] Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China

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

来源：

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES | 2025年 / 279卷 / 01期

基金：

中国国家自然科学基金;

关键词：

MAGNETIZED NEUTRON-STARS; ACTIVE EPISODE; GRB; 221009A; LONG; VARIABILITY; EMISSION; GECAM; PERFORMANCE; CALIBRATION; DISCOVERY;

D O I：

10.3847/1538-4365/addb42

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

SGR J1935+2154 is an extremely active magnetar and the source of the first fast radio burst in the Milky Way, characterized as a magnetar X-ray burst, but whether the temporal features of this magnetar are specific or not is not well known. Based on data from the Fermi Gamma-ray Burst Monitor (GBM), Gravitational Wave High-energy Electromagnetic Counterpart All-Sky Monitor (GECAM), and Hard X-ray Modulation Telescope (HXMT), we investigate the temporal properties of pulses and bursts, covering parameters such as the minimum variability timescale (MVT), duration, rise/decay/waiting times, skewness, peakedness, pulse width, and number of pulses. Except for the number of pulses, all parameters follow the log-Gaussian distribution. In the GBM and GECAM data, MVT and duration exhibit a negative correlation, while the number of pulses and duration (or MVT) exhibit a positive (or negative) correlation. Universal power-law relationships exist among parameters, for example, rise time is positively correlated with decay time, while decay/rise time (or width) and peakedness show a negative correlation. We did not find a significant difference compared with another magnetar, SGR J0501+4516. Finally, the parameters observed by GBM and GECAM show no significant differences, but some parameters observed by HXMT differ from both, suggesting that they may originate from a different physical mechanism.

引用

页数：13

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