SXP 31.0 -- 小麦哲尔云中持续26年的宁静期后2025年接近爱丁顿极限的双X射线爆发
SXP 31.0 -- the 2025 near-Eddington double X-ray outburst after 26 years of quiescence
AI总结：
SXP 31.0在2025年经历罕见的两次背靠背型II爆发，其亮度接近爱丁顿极限，首次发现其周围晕轮可能为巧合的HII区域。
摘要：
SXP 31.0是位于小麦哲尔云（SMC）中的X射线源，1998年首次被识别为一个Be X射线双星（BeXRB）系统。现在已知其由一颗OBe主序星和一个自转周期为31秒的中子星组成。2025年，该源开始新的X射线爆发阶段，其亮度接近10^38 erg/s的爱丁顿极限。异常的是，H-α图像显示其周围有一个晕轮，其性质尚不明确。在本文中，我们报告了该晕轮的新观测结果，包括首次多纤维积分光度单位（IFU）观测，将该发射识别为可能的巧合HII区域。X射线、紫外和光学数据覆盖约200天，揭示该源在2025年经历了两次明亮的背靠背型II爆发，这在任何BeXRB系统中都是罕见的。
英文摘要：
SXP 31.0 is an X-ray source in the Small Magellanic Cloud (SMC) that was first identified as a Be X-ray Binary (BeXRB) system when it went into X-ray outbusrst in 1998. It is now known to consist of an OBe main sequence star and a neutron star with a spin period of 31s. In 2025 a new X-ray outburst phase began with the source exhibiting a luminosities approaching the Eddington limit of 10^38 erg/s. Unusually, H-alpha images show it has a surrounding halo whose nature has not been clear. In this paper, we report new observations of this halo, including the first multi-fibre Integrated Flux Unit (IFU) observations, which identify this emission as probably a coincidental HII region. The X-ray, UV & optical data cover a period of ~200d and reveal that the source underwent two bright, back-to-back, Type II outbursts in 2025 - a rare occurrence for any BeXRB system.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
