论文标题
AMXP IGR J17591-2342的光谱分析在其2018年爆发期间
Spectral analysis of the AMXP IGR J17591-2342 during its 2018 outburst
论文作者
论文摘要
积累毫秒的X射线脉冲脉冲IGR J17591-2342是一种LMXB系统，于2018年8月爆发，由较好的天文台监视，部分由其他设施进行了监控。我们旨在通过利用同时观察的整个X射线数据存储库来研究该来源在爆发过程中的光谱发射如何演变。平均而言，合并的宽带光谱的连续发射通过吸收的组合成分散射黑体散射的黑体散射光子在（0.8 +/- 0.5）keV处峰值，通过中等光学厚的Corona（TAU = 2.3 +/- 0.5），温度为（34 +/- 9）kev。某些光谱需要温度和径向尺寸为（0.8 +/- 0.2）keV和（3.3 +/- 1.5）km的黑体分量（3.3 +/- 1.5）km，这表明中央发射的一部分可能是中子星表面的一部分，并未有效地散布在Corona中。低能量处的连续体的特征是显着残留物，表明存在O VIII的吸收边缘和NE IX离子的发射线。此外，在爆发的不同时间检测到宽Fe I和Fe XXV K-Alpha发射线，表明系统中存在反射。
The Accreting Millisecond X-ray Pulsar IGR J17591-2342 is a LMXB system that went in outburst on August 2018 and it was monitored by the NICER observatory and partially by other facilities. We aim to study how the spectral emission of this source evolved during the outburst, by exploiting the whole X-ray data repository of simultaneous observations. The continuum emission of the combined broad-band spectra is on average well described by an absorbed Comptonisation component scattering black-body-distributed photons peaking at (0.8+/-0.5) keV, by a moderately optically thick corona (tau=2.3+/-0.5) with temperature of (34+/-9) keV. A black-body component with temperature and radial size of (0.8+/-0.2) keV and (3.3+/-1.5) km respectively is required by some of the spectra and suggests that part of the central emission, possibly a fraction of the neutron star surface, is not efficiently scattered by the corona. The continuum at low energies is characterised by significant residuals suggesting the presence of an absorption edge of O VIII and of emission lines of Ne IX ions. Moreover, broad Fe I and Fe XXV K-alpha emission lines are detected at different times of the outburst, suggesting the presence of reflection in the system.
