论文标题
解开附近的脉冲星SXP 15.3和SXP 305
Disentangling the neighbouring pulsars SXP 15.3 and SXP 305
论文作者
论文摘要
SXP 15.3和SXP 305是两个是X射线二进制文件，在小麦芽云中，在空间上被〜7 Arcsec分离。过去，这些来源之间的小分离导致对联合区域发射的起源产生混乱。我们介绍了两个来源的长期光学和X射线监测结果，我们研究了历史性和最近的行为。特别是，从作为S-tep项目的一部分收集的数据中，我们可以看到在尼尔·盖尔斯·斯威夫特（Neil Gehrels Swift）的近期光曲线中重复从两个来源的联合区域中重复X射线爆发，我们研究了这种排放的起源。使用来自南部非洲大型望远镜（盐）的H-α发射线和光学引力透镜实验（OGLE）的光度通量来研究BE DISC的大小和结构的变化，我们证明X射线发射可能起源于SXP 15.3。定时分析揭示了异常的行为，其中光爆发曲线显示了X射线爆发频率的两倍的调制。我们认为，这两个周期性是SXP 15.3中的真实轨道时期，并根据BE DISC和中子星的几何取向提出模型，以解释爆发的物理起源。
SXP 15.3 and SXP 305 are two Be X-ray binaries in the Small Magellanic Cloud that are spatially separated by ~7 arcsec. The small separation between these sources has, in the past, resulted in confusion about the origin of the emission from the combined region. We present long-term optical and X-ray monitoring results of both sources, where we study the historic and recent behaviour. In particular, from data collected as part of the S-CUBED project we see repeating X-ray outbursts from the combined region of the two sources in the recent lightcurve from the Neil Gehrels Swift Observatory, and we investigate the origin of this emission. Using the H-alpha emission line from the Southern African Large Telescope (SALT) and photometric flux from the Optical Gravitational Lensing Experiment (OGLE) to study the changes in the size and structure of the Be disc, we demonstrate that the X-ray emission likely originates from SXP 15.3. Timing analysis reveals unusual behaviour, where the optical outburst profile shows modulation at twice the frequency of the X-ray outbursts. We consider either of these periodicities being the true orbital period in SXP 15.3 and propose models based on the geometric orientations of the Be disc and neutron star to explain the physical origin of the outbursts.
