Alive but Barely Kicking: 来自Swift与XMM-Newton对eRO-QPE1准周期爆发3年多X射线监测的新消息
Alive but Barely Kicking: News from 3+ years of Swift and XMM-Newton X-ray Monitoring of Quasi-Periodic Eruptions from eRO-QPE1
AI总结：
本研究通过三年多的Swift X射线监测追踪eRO-QPE1的准周期爆发，发现其复发时间在0.6-1.2天波动、无长期演化趋势，爆发峰值流量持续下降至近不可测，因背景光度低于探测限无法验证其与流量减弱的关联，为QPE物理机制研究提供了长时标演化新数据。
摘要：
准周期爆发（Quasi-periodic Eruptions, QPEs）是一类新型河外X射线暂现源，已知其会以数小时至数天的大致规则间隔重复发生。其潜在物理机制是热议的话题，多数模型提出它们要么起源于内吸积流内部的不稳定性，要么来自轨道运行的天体。目前，除了独特的QPE源GSN 069之外，我们对QPEs在多年的长时标下如何演化的认知十分有限。本研究中，我们展示了过去三年间策略性设计的Swift观测项目的结果，该项目旨在追踪eRO-QPE1的爆发。我们的主要结果如下：1）爆发的复发时间在0.6至1.2天之间变化；2）复发时间的演化未检测到长期趋势；3）与既往研究一致，其爆发轮廓可具有复杂形状；4）过去三年间爆发的峰值流量持续下降，在2023年6月获取的最新Swift数据集中几乎检测不到爆发。这种爆发减弱的趋势近期已在GSN 069中被报道。然而，由于eRO-QPE1的背景光度低于我们的探测极限，我们无法验证这种减弱是否与背景光度相关（据称GSN 069中存在这种相关性）。我们在多种已提出的QPE模型的背景下讨论了这些发现。
英文摘要：
Quasi-periodic Eruptions (QPEs) represent a novel class of extragalactic X-ray transients that are known to repeat at roughly regular intervals of a few hours to days. Their underlying physical mechanism is a topic of heated debate, with most models proposing that they originate either from instabilities within the inner accretion flow or from orbiting objects. At present, our knowledge of how QPEs evolve over an extended timescale of multiple years is limited, except for the unique QPE source GSN 069. In this study, we present results from strategically designed Swift observing programs spanning the past three years, aimed at tracking eruptions from eRO-QPE1. Our main results are: 1) the recurrence time of eruptions can vary between 0.6 and 1.2 days, 2) there is no detectable secular trend in evolution of the recurrence times, 3) consistent with prior studies, their eruption profiles can have complex shapes, and 4) the peak flux of the eruptions has been declining over the past 3 years with the eruptions barely detected in the most recent Swift dataset taken in June of 2023. This trend of weakening eruptions has been reported recently in GSN 069. However, because the background luminosity of eRO-QPE1 is below our detection limit, we cannot verify if the weakening is correlated with the background luminosity (as is claimed to be the case for GSN 069). We discuss these findings within the context of various proposed QPE models.
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