发表机构
Guangxi University; Purple Mountain Observatory, Chinese Academy of Sciences; University of Science and Technology of China（广西大学; 中国科学院紫金山天文台; 中国科学技术大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
该研究通过同时观测的伽马射线脉冲与X射线耀斑对，发现两者时间参数和各向同性能量呈相似幂律分布，支持它们具有共同物理起源。
AI 中文摘要
X射线耀斑的统计性质与伽马射线暴（GRB）瞬时辐射的统计性质高度相似，表明它们可能具有共同的物理起源（例如中心引擎活动）。然而，对非同时观测的余辉X射线耀斑和瞬时伽马射线脉冲进行的可比统计研究仍不完整。本文通过系统搜索与X射线耀斑同时发生的伽马射线辐射，识别出38个包含50个脉冲-耀斑对的GRB，其中19个具有测量的红移。我们在它们重叠的时间间隔内对伽马射线脉冲和X射线耀斑进行了联合的时间和光谱分析，发现每对的光谱可以用吸收幂律（PL）、PL加黑体（PL+BB）、截断幂律（CPL）和Band函数很好地描述。更重要的是，通过对瞬时伽马射线脉冲和同时观测到的X射线耀斑应用自组织临界性（SOC）分析，我们发现这两个分量的时间参数（例如等待时间、上升时间、峰值时间、衰减时间和持续时间）遵循相似的幂律分布，其中等待时间的最大绝对差为Δα~0.36，而其他四个参数的差异要小得多（Δα≲0.12）。对于从具有测量红移的子样本导出的各向同性能量，两个分量之间的差异为Δα~0.54。这些结果表明，X射线耀斑和瞬时辐射可能具有相同的物理起源。
英文摘要
Statistical properties of X-ray flares are highly similar to those of the prompt emission in gamma-ray bursts (GRBs), suggesting that they may share a common physical origin (e.g., central engine activity). However, comparable statistical studies of afterglow X-ray flares and prompt gamma-ray pulses that are not observed simultaneously remain incomplete. In this paper, by systematically searching for gamma-ray emission simultaneous with X-ray flares, we identify 38 GRBs containing 50 pulse--flare pairs, 19 of which have measured redshifts. We perform joint temporal and spectral analyses of the gamma-ray pulses and X-ray flares over their overlapping time intervals, and find that the spectrum of each pair can be well described by an absorbed power-law (PL), PL plus blackbody (PL+BB), cutoff power-law (CPL), and Band function. More importantly, by applying self-organized criticality (SOC) analysis to both the prompt gamma-ray pulses and the simultaneously observed X-ray flares, we find that the temporal parameters (e.g., waiting time, rise time, peak time, decay time, and duration) of the two components follow similar power-law distributions, with the largest absolute difference of $Δα\sim0.36$ for the waiting time and much smaller differences ($Δα\lesssim0.12$) for the other four parameters. For the isotropic energy derived from the subsample with measured redshifts, the difference between the two components is $Δα\sim0.54$. These results suggest that the X-ray flares and the prompt emission are likely to share the same physical origin.
Comments14 pages, 2 tables, and 6 figures. Accepted for publication in ApJ, and matched with the published verison
Journal refThe Astrophysical Journal, 1008, 103 (2026)
