论文标题
Swift揭示了IGR J18214-1318的轨道时期
Swift unveils the orbital period of IGR J18214-1318
论文作者
论文摘要
我们分析了在高质量X射线二元IGR J18214-1318上收集的尼尔·盖尔斯（Neil Gehrels）Swift天文台调查数据的13年。进行时间分析，我们检测到5.42 d的周期性信号。从伴侣星特性中，我们得出了$ \ sim 41 \ rm r _ {\ odot} \ simeq 2 r _ {\ star} $的平均轨道分离。伴侣恒星（O9）的光谱类型和紧密的轨道分离表明IGR〜J18214-1318是一种偏心率低于0.17的风源。在轨道时期折叠的强度曲线显示出与伴侣恒星的最小兼容。此外，我们使用XMM-Newton，Nustar和Swift的数据报告了宽带0.6--100 KEV频谱，并应用了自洽的物理模型。我们发现，频谱通过纯的热构成组件很好地拟合，或者假设源是由组合的热和散装构成模型的中子恒星积聚在临界方案之上的中子恒星。在这两种情况下，都需要存在局部中性吸收（可能与伴侣恒星的厚风有关）。
We analysed 13 years of the Neil Gehrels Swift Observatory survey data collected on the High Mass X-ray Binary IGR J18214-1318. Performing the timing analysis we detected a periodic signal of 5.42 d. From the companion star characteristics we derived an average orbital separation of $\sim 41 \rm R_{\odot}\simeq 2 R_{\star}$. The spectral type of the companion star (O9) and the tight orbital separation suggest that IGR~J18214-1318 is a wind accreting source with eccentricity lower than 0.17. The intensity profile folded at the orbital period shows a deep minimum compatible with an eclipse of the source by the companion star. In addition, we report on the broad-band 0.6--100 keV spectrum using data from XMM-Newton, NuSTAR, and Swift, applying self-consistent physical models. We find that the spectrum is well fitted either by a pure thermal Comptonization component, or, assuming that the source is a neutron star accreting above the critical regime, by a combined thermal and bulk-motion Comptonization model. In both cases, the presence of a local neutral absorption (possibly related to the thick wind of the companion star) is required.
