An XMM-Newton observation of the symbiotic star AG Peg: The X-ray emission after the end of its 2015 outburst

被引：0
作者：
Zhekov S.A. [1 ]
Tomov T.V. [2 ]
机构：
[1] Institute of Astronomy and National Astronomical Observatory (Bulgarian Academy of Sciences), 72 Tsarigradsko Chaussee Blvd., Sofia
[2] Centre for Astronomy, Faculty of Physics, Astronomy, and Informatics, Nicolaus Copernicus University, Grudziadzka 5, Torun
来源：
Zhekov, Svetozar A. (szhekov@astro.bas.bg) | 2018年 / Oxford University Press卷 / 481期
基金：
美国国家航空航天局;
关键词：
Binaries: symbiotic; Shock waves; Stars: individual: AGPeg; X-rays: stars;
D O I：
10.1093/MNRAS/STY2644
中图分类号：
学科分类号：
摘要：
We present an analysis of the XMM-Newton observation of the symbiotic starAG Peg, obtained after the end of its 2015 outburst. The X-ray emission of AGPeg is soft and of thermal origin. AGPeg is an X-ray source of class β of the X-ray sources among the symbiotic stars, whose X-ray spectrum is well matched by a two-temperature optically thin plasma emission (kT1 ~ 0.14 keV and kT2 ~ 0.66 keV). The X-ray emission of the class β sources is believed to originate from colliding stellar winds (CSWs) in a binary system. If we adopt the CSW picture, the theoretical CSW spectra match well the observed properties of the XMM-Newton spectra of AGPeg. However, we need a solid evidence that a massive-enough hot-star wind is present in the post-outburst state of AGPeg to proof the validity of the CSW picture for this symbiotic binary. No short-term X-ray variability is detected while the UV emission of AGPeg shows stochastic variability (flickering) on time-scales of minutes and hours. © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
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页码：5156 / 5162
页数：6
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