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首页> 外文期刊>Astronomy and astrophysics >Spectral evolution of the supergiant HMXB IGR J16320–4751 along its orbit using XMM-Newton
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Spectral evolution of the supergiant HMXB IGR J16320–4751 along its orbit using XMM-Newton

机译：使用 XMM-Newton ，超巨型HMXB IGR J16320–4751沿其轨道的光谱演化

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Context . The INTEGRAL satellite has revealed a previously hidden population of absorbed high-mass X-ray binaries (HMXBs) hosting supergiant stars. Among them, IGR J16320–4751 is a classical system intrinsically obscured by its environment, with a column density of ～10~(23)cm~(?2), more than an order of magnitude higher than the interstellar absorption along the line of sight. It is composed of a neutron star rotating with a spin period of ～1300 s, accreting matter from the stellar wind of an O8I supergiant star, with an orbital period of ～9 days. Aims . We investigated the geometrical and physical parameters of both components of the binary system IGR J16320–4751. Since in systems of this type the compact object is usually embedded in the dense and powerful wind of an OB supergiant companion, our main goal here was to study the dependence of the X-ray emission and column density along the full orbit of the neutron star around the supergiant star. Methods . We analyzed all existing archival XMM-Newton and Swift /BAT observations collected between 2003 and 2008, performing a detailed temporal and spectral analysis of the X-ray emission of the source. We then fitted the parameters derived in our study, using a simple model of a neutron star orbiting a supergiant star. Results . The XMM-Newton light curves of IGR J16320–4751 display high-variability and flaring activity in X-rays on several timescales, with a clear spin period modulation of ～1300 s. In one observation we detected two short and bright flares where the flux increased by a factor of ～10 for ～300 s, with similar behavior in the soft and hard X-ray bands. By inspecting the 4500-day light curves of the full Swift /BAT data, we derived a refined period of 8.99??±??0.01 days, consistent with previous results. The XMM-Newton spectra are characterized by a highly absorbed continuum and an Fe absorption edge at ～7 keV. We fitted the continuum with a thermally comptonized COMPTT model, and the emission lines with three narrow Gaussian functions using two TBABS absorption components, to take into account both the interstellar medium and the intrinsic absorption of the system. For the whole set of observations we derived the column density at different orbital phases, showing that there is a clear modulation of the column density with the orbital phase. In addition, we also show that the flux of the Fe K α line is correlated with the N _(H)column, suggesting a clear link between absorbing and fluorescent matter that, together with the orbital modulation, points towards the stellar wind being the main contributor to both continuum absorption and Fe K α line emission. Conclusions . Assuming a simple model for the supergiant stellar wind we were able to explain the orbital modulation of the absorption column density, Fe K α emission and the high-energy Swift /BAT flux, allowing us to constrain the geometrical parameters of the binary system. Similar studies applied to the analysis of the spectral evolution of other sources will be useful to better constrain the physical and geometrical properties of the sgHMXB class.
机译：语境。 INTEGRAL卫星显示了先前隐藏的大量吸收了超大质量恒星的高吸收X射线双星（HMXB）。其中，IGR J16320–4751是一个典型的经典系统，其环境本质上被其环境所遮蔽，其列密度约为10〜（23）cm〜（？2），比沿星际线的星际吸收高一个数量级。视线。它由一个自旋周期为〜1300 s的中子星组成，从O8I超巨型恒星的恒星风中吸收物质，其轨道周期为〜9天。目的。我们研究了二元系统IGR J16320–4751的两个组件的几何和物理参数。由于在这种类型的系统中，紧凑的物体通常嵌入在OB超巨伴的密集而强大的风中，因此我们的主要目标是研究沿着中子星整个轨道的X射线发射和列密度的依赖性。围绕着超级巨星。方法 。我们分析了2003年至2008年之间收集的所有现有XMM-Newton档案和Swift / BAT观测资料，并对源的X射线发射进行了详细的时间和光谱分析。然后，我们使用绕超巨星运行的中子星的简单模型拟合了研究中得出的参数。结果。 IGR J16320–4751的XMM-牛顿光曲线在多个时间尺度上均表现出高可变性和X射线耀斑活动，自旋周期调制约为1300 s。在一项观测中，我们检测到两个短而明亮的耀斑，其中通量在〜300 s内增加了〜10倍，在软X射线和硬X射线带中行为相似。通过检查完整的Swift / BAT数据的4500天光曲线，我们得出了8.99±±0.01天的精确周期，与以前的结果一致。 XMM-牛顿光谱的特征是具有高吸收的连续峰和〜7 keV的Fe吸收边。我们使用热补偿COMPTT模型对连续体进行拟合，并使用两个TBABS吸收分量将发射谱线具有三个窄高斯函数，以同时考虑星际介质和系统的固有吸收。对于整个观测，我们得出了在不同轨道相位下的柱密度，这表明柱密度明显受到轨道相位的调节。此外，我们还表明，Fe Kα线的通量与N _（H）柱相关，这表明吸收和荧光物质之间存在明确的联系，与轨道调制一起，指向恒星风是连续吸收和Fe Kα谱线发射的主要贡献者。结论。假设超级恒星风的简单模型，我们能够解释吸收柱密度，Fe Kα发射和高能Swift / BAT通量的轨道调制，从而使我们能够限制二元系统的几何参数。应用于其他来源的光谱演化分析的类似研究将有助于更好地限制sgHMXB类的物理和几何特性。

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