磁星爆发脉冲的自组织临界行为

Shuo Xiao, Mei-Xin Hong, Zi-Yi You, Tong-Lei Liao, Shao-Lin Xiong, Shu-Xu Yi, Ping Wang, Jiao-Jiao Yang, Zheng-Huo Jiang, Yue Wang, Yan-Qiu Zhang, Ming-Yu Ge, Zhen Zhang, Xi-Hong Luo, Shi-Jun Dang, Ru-shuang Zhao, Ai-Jun Dong, Qi-Jun Zhi, He Gao, Di Li, Shuang-Nan Zhang
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引用次数: 0

摘要

源于磁星的 X 射线暴(XRBs)的整体时间和光谱特征(如持续时间、通量、峰值通量、峰值计数率和总计数)已得到广泛研究,以证实其自组织临界(SOC)行为。然而,XRB 中的脉冲是揭示磁重联和地壳破裂等辐射过程的重要部分,其可变的统计特征仍不清楚。在这项工作中,我们研究了费米伽马射线暴监测仪、Insight-HXMT 和 GECAM 观测到的两个活跃而多产的磁星 SGR J1935+2154 和 SGR J1550-5418 的脉冲持续时间、等待时间、峰值计数率和脉冲串总计数的波动分布。我们报告说,脉冲的等待时间与 SOC 一致,而以前的研究表明脉冲串的等待时间与 SOC 不一致,这可能是由于观测不完整造成的。此外,脉冲的持续时间、峰值计数率和总计数也是 SOC 行为。我们的发现为脉冲串中每个辐射过程的 SOC 提供了证据,例如,由单个星震引发的多次磁重联产生的多个脉冲串。最后,来自两颗磁星的脉冲具有相似的统计特征,这为它们的共同辐射过程提供了支持。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
The Self-organized Criticality Behaviors of Pulses in Magnetar Bursts
The overall temporal and spectral characteristics (e.g., duration, fluence, peak flux, peak count rate, and total counts) of X-ray bursts (XRBs) originating from magnetars have been extensively studied to confirm their self-organized criticality (SOC) behaviors. However, for the pulses in XRBs, which are an important part of unraveling radiation processes such as magnetic reconnection and crustal rupture, their variable statistical characteristics are still unclear. In this work, we investigate the distributions of fluctuations in duration, waiting time, peak count rate, and total counts of pulses within bursts from two active and prolific magnetars, SGR J1935+2154 and SGR J1550-5418, observed by Fermi’s Gamma-ray Burst Monitor, Insight-HXMT, and GECAM. We report that the waiting time for pulses follows SOC, whereas previous studies indicated for bursts do not, possibly due to incomplete observations. Besides, the duration, peak count rate, and total counts for pulses are also SOC behaviors. The α-values for the duration of pulses for both magnetars are ∼2, and the inferred Euclidean dimension S is 3. Our findings provide evidence for the SOC of each radiation process during a burst, for example, multiple pulses produced by multiple magnetic reconnections triggered by a single starquake. Finally, the similar statistical characteristics for pulses from both magnetars lend support to their shared radiation processes.
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