X-ray emission from O-type stars: DH Cep and HD 97434

被引：9
作者：
Bhatt, Himali [1 ]
Pandey, J. C. [1 ]
Kumar, Brijesh [1 ]
Sagar, Ram [1 ]
Singh, K. P. [2 ]
机构：
[1] Aryabhatta Res Inst Observat Sci, Naini Tal 263129, Uttarakhand, India
[2] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India
来源：
NEW ASTRONOMY | 2010年 / 15卷 / 08期
关键词：
Star:X-ray; Star:binary; Star:wind; Star:individual (DH Cep and HD 97434); XMM-NEWTON VIEW; ABSORPTION; WINDS; SPECTROSCOPY; TEMPERATURES; EINSTEIN; CYG;
D O I：
10.1016/j.newast.2010.04.001
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We present X-ray emission characteristics of the massive O-type stars DH Cep and HD 97434 using archival XMM-Newton observations. There is no convincing evidence for short-term variability in the X-ray intensity during the observations. However, the analysis of their spectra reveals X-ray structure being consistent with two-temperature plasma model. The hydrogen column densities derived from X-ray spectra of DH Cep and HD 97434 are in agreement with the reddening measurements for their corresponding host clusters NGC 7380 and Trumpler 18, indicating that the absorption by stellar wind is negligible. The X-ray emission from these hot stars is interpreted in terms of the standard instability-driven wind-shock model. (C) 2010 Elsevier B.V. All rights reserved.
引用
收藏
页码：755 / 759
页数：5
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