讨论4U 1538-52中2.1 keV吸收特性的物理意义
Discussing the physical meaning of the absorption feature at 2.1 keV in 4U 1538-52
摘要：
高分辨X射线能谱是研究X射线双星中中子星周围物质的性质及其与星风相互作用的有力工具。特别是，它们光谱中的吸收特征可以揭示中子星大气层的存在或它们的磁场强度。在这里，我们提出了在2.1 keV的高质量X射线双星4U 1538-52的X射线光谱的吸收功能的调查，根据我们以前的分析XMM-牛顿数据。我们研究了各种可能的起源，并讨论了不同的物理场景，以解释这一特点。一个可能的解释是，这个特征与O/Ne中子星大气中的原子跃迁有关，或者与施主星风中形成的氢和氦（如Fe或Si离子）有关。
英文摘要：
High resolution X-ray spectroscopy is a powerful tool for studying the nature of the matter surrounding the neutron star in X-ray binaries and its interaction between the stellar wind and the compact object. In particular, absorption features in their spectra could reveal the presence of atmospheres of the neutron star or their magnetic field strength. Here we present an investigation of the absorption feature at 2.1 keV in the X-ray spectrum of the high mass X-ray binary 4U 1538-52 based on our previous analysis of the XMM-Newton data. We study various possible origins and discuss the different physical scenarios in order to explain this feature. A likely interpretation is that the feature is associated with atomic transitions in an O/Ne neutron star atmosphere or of hydrogen and helium like Fe or Si ions formed in the stellar wind of the donor.
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