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

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

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),...

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Main Authors: Jiao-Jiao Yang, Shuo Xiao, Yue Wang, Shao-Lin Xiong, Lin Lin, Zheng-Huo Jiang, Tong-Lei Liao, Xiao-Bo Li, Cheng-Kui Li, Shu-Xu Yi, Zhen Zhang, Shuang-Nan Zhang
Format: Article
Language:English
Published: IOP Publishing 2025-01-01
Series:The Astrophysical Journal Supplement Series
Subjects:
Magnetars
Online Access:https://doi.org/10.3847/1538-4365/addb42
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Summary: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.
ISSN:0067-0049

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