Unveil A Peculiar Light Curve Pattern of Magnetar Burst with GECAM observations of SGR J1935+2154
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| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| _version_ | 1866918159465840640 |
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| author | Wang, Yue Wang, Chen-Wei Xiong, Shaolin Xiao, Xiao Zhang, Yanqiu Xie, Sheng-Lun Lin, Lin Yang, Yuan-Pei Guo, Haoxuan Cai, Ce Huang, Yue Li, Cheng-Kui Li, Bing Li, Xiaobo Liu, Jiacong Ma, Xiang Song, Liming Tan, Wen-Jun Wang, Ping Xue, Wang-Chen Yi, Shu-Xu Yu, Yun-Wei Yu, Zheng-Hang Zhang, Jin-Peng Zhang, Peng Zhang, Shuang-Nan Zhang, Wen-Long Zhang, Zhen Zhao, Xiao-Yun Zheng, Chao Zheng, S. J. |
| author_facet | Wang, Yue Wang, Chen-Wei Xiong, Shaolin Xiao, Xiao Zhang, Yanqiu Xie, Sheng-Lun Lin, Lin Yang, Yuan-Pei Guo, Haoxuan Cai, Ce Huang, Yue Li, Cheng-Kui Li, Bing Li, Xiaobo Liu, Jiacong Ma, Xiang Song, Liming Tan, Wen-Jun Wang, Ping Xue, Wang-Chen Yi, Shu-Xu Yu, Yun-Wei Yu, Zheng-Hang Zhang, Jin-Peng Zhang, Peng Zhang, Shuang-Nan Zhang, Wen-Long Zhang, Zhen Zhao, Xiao-Yun Zheng, Chao Zheng, S. J. |
| contents | Magnetar X-ray Burst (MXB) is usually composed of a single pulse or multiple pulses with rapid rise and brief duration mostly observed in hard X-ray (soft gamma-ray) band. Previous work studied the temporal behavior of some magnetar bursts and employed the Fast Rise Exponential Decay (FRED) model to fit pulses of MXB. However, whether there is other kind of pulse shape has not been explored. In this study, we systematically examined light curve of MXBs from SGR J1935+2154 detected by GECAM between 2021 and 2022. We find that there are different light curve morphologies. Especially, we discover a peculiar and new pattern, Exponential Rise and Cut-Off Decay (ERCOD), which is significantly different from FRED and could be well described by a mathematical function we proposed. We find that MXBs with ERCOD shape are generally longer in duration, brighter in the peak flux, and harder in spectrum. We note that the ERCOD shape is not unique to SGR J1935+2154 but also present in other magnetars. This new light curve pattern may imply a special burst and radiation mechanism of magnetar. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2510_11385 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Unveil A Peculiar Light Curve Pattern of Magnetar Burst with GECAM observations of SGR J1935+2154 Wang, Yue Wang, Chen-Wei Xiong, Shaolin Xiao, Xiao Zhang, Yanqiu Xie, Sheng-Lun Lin, Lin Yang, Yuan-Pei Guo, Haoxuan Cai, Ce Huang, Yue Li, Cheng-Kui Li, Bing Li, Xiaobo Liu, Jiacong Ma, Xiang Song, Liming Tan, Wen-Jun Wang, Ping Xue, Wang-Chen Yi, Shu-Xu Yu, Yun-Wei Yu, Zheng-Hang Zhang, Jin-Peng Zhang, Peng Zhang, Shuang-Nan Zhang, Wen-Long Zhang, Zhen Zhao, Xiao-Yun Zheng, Chao Zheng, S. J. High Energy Astrophysical Phenomena Magnetar X-ray Burst (MXB) is usually composed of a single pulse or multiple pulses with rapid rise and brief duration mostly observed in hard X-ray (soft gamma-ray) band. Previous work studied the temporal behavior of some magnetar bursts and employed the Fast Rise Exponential Decay (FRED) model to fit pulses of MXB. However, whether there is other kind of pulse shape has not been explored. In this study, we systematically examined light curve of MXBs from SGR J1935+2154 detected by GECAM between 2021 and 2022. We find that there are different light curve morphologies. Especially, we discover a peculiar and new pattern, Exponential Rise and Cut-Off Decay (ERCOD), which is significantly different from FRED and could be well described by a mathematical function we proposed. We find that MXBs with ERCOD shape are generally longer in duration, brighter in the peak flux, and harder in spectrum. We note that the ERCOD shape is not unique to SGR J1935+2154 but also present in other magnetars. This new light curve pattern may imply a special burst and radiation mechanism of magnetar. |
| title | Unveil A Peculiar Light Curve Pattern of Magnetar Burst with GECAM observations of SGR J1935+2154 |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2510.11385 |