White dwarf masses in intermediate polars observed with the Suzaku satellite
White dwarf masses in intermediate polars observed with the Suzaku satellite
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DOI：
10.1051/0004-6361/201014542
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发表时间：
2010-06
影响因子：
6.5
通讯作者：
T. Yuasa;K. Nakazawa;K. Makishima;Kei Saitou;M. Ishida;K. Ebisawa;H. Mori;S. Yamada
中科院分区：
文献类型：
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作者：
T. Yuasa;K. Nakazawa;K. Makishima;Kei Saitou;M. Ishida;K. Ebisawa;H. Mori;S. Yamada
上下文激变变星中的白色矮星是重要的实验室，在那里电子简并在宏观尺度上发生。由于敏感的硬X射线任务，磁CV的数量增加，特别是在硬X射线波段（10 keV）。目标。从X射线光谱学，我们估计了中等磁化CV或中间极性（IP）中附近WD的质量。方法.使用朱雀卫星，我们获得了17个IP的宽带光谱，覆盖3 - 50 keV。利用Suleimanov等人（2005，A&A，435，191）的吸积柱模型和光学薄热发射程序，建立了具有分辨Fe发射线的离子聚合物的光谱发射模型。通过同时拟合Fe线络合物和硬X射线连续谱，确定了冲击温度和WD质量，其精度比以往的研究更好。
Context. White dwarfs (WDs) in cataclysmic variables (CVs) are important experimental laboratories where the electron degeneracy is taking place on a macroscopic scale. Magnetic CVs increase in number especially in the hard X-ray band (10 keV) thanks to sensitive hard X-ray missions. Aims. From X-ray spectroscopy, we estimate the masses of nearby WDs in moderately-magnetized CVs, or Intermediate Polars (IPs). Methods. Using the Suzaku satellite, we aquired wide-band spectra of 17 IPs, covering 3−50 keV. An accretion column model of Suleimanov et al. (2005, A&A, 435, 191) and an optically-thin thermal emission code were used to construct a spectral emission model of IPs with resolved Fe emission lines. By simultaneously fitting the Fe line complex and the hard X-ray continuum of individual spectra, the shock temperature and the WD mass were determined with a better accuracy than in previous studies.