The masses of hot subdwarfs
The masses of hot subdwarfs
复制标题
大量热亚矮星
DOI：
10.1051/0004-6361/200912336
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发表时间：
2009-09
期刊：
影响因子：
--
通讯作者：
陈雪飞
中科院分区：
文献类型：
--
作者：
张先飞;韩占文;陈雪飞
背景。质量是一个基本参数，但对于大多数热亚矮星来说，其质量并不为人们所熟知。一般而言，热亚矮星的质量是通过星震学或动力学方法推导出来的，而通常很难从这些方法中获取必要的数据。
Context. Masses are a fundamental parameter, but they are not well known for most hot subdwarfs. In general, the mass of a hot subdwarf is derived with asteroseismology or dynamical methods, for which it is often difficult to obtain the necessary data from observations. Aims. We intend to find an approach to deriving the masses of hot subdwarfs from observational data in the literature. Methods. We presented full evolutionary calculations for hot subdwarfs in a wide mass range (0.33 M(circle dot) to 1.4 M(circle dot)) for a Population I metallicity of Z = 0.02, and obtained a relation between M(p) and log (T(eff)(4)/g), where M(p), T(eff), and g are the most probable mass, effective temperature, and gravity. This relation is used to study the masses of some observed hot subdwarfs. Results. We proposed a method of determining the masses of hot subdwarfs. Using this method, we studied the masses of hot subdwarfs from the ESO supernova Ia progenitor survey and Hamburg quasar survey. The study shows that most of subdwarf B stars have masses between 0.42 and 0.54 M(circle dot), whilst most sdO stars are in the range 0.40 similar to 0.55 M(circle dot). Comparing our study to the theoretical mass distributions of Han et al. (2003, MNRAS, 341, 669), we found that sdO stars with mass less than similar to 0.5 M(circle dot) may evolve from sdB stars, whilst most high-mass(>0.5 M(circle dot)) sdO stars result from mergers directly.
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DOI：
10.1046/j.1365-8711.2001.04376.x
发表时间：
2000-08
期刊：
--
影响因子：
--
作者：
C. Pearson;H. Matsuhara;H. Watarai;T. Matsumoto;T. Onaka
通讯作者：
C. Pearson;H. Matsuhara;H. Watarai;T. Matsumoto;T. Onaka
DOI：
10.1046/j.1365-8711.2002.05752.x
发表时间：
2002-06
影响因子：
4.8
作者：
Zhanwen Han;P. Podsiadlowski;P. Maxted;T. Marsh;N. Ivanova
通讯作者：
Zhanwen Han;P. Podsiadlowski;P. Maxted;T. Marsh;N. Ivanova
影响因子：
4.8
作者：
K. Schröder;O. Pols;P. Eggleton
通讯作者：
K. Schröder;O. Pols;P. Eggleton
DOI：
10.1111/j.1365-2966.2001.04714.x
发表时间：
2001-03
影响因子：
4.8
作者：
P. Maxted;U. Heber;T. Marsh;R. S. U. O. Southampton;Keele University;Astronomisches Institut der Universitat Erlangen-Nurnberg-Astronomisch
通讯作者：
P. Maxted;U. Heber;T. Marsh;R. S. U. O. Southampton;Keele University;Astronomisches Institut der Universitat Erlangen-Nurnberg-Astronomisch
DOI：
10.1111/j.1365-2966.2007.12151.x
发表时间：
2006-12
期刊：
Proceedings of the International Astronomical Union
影响因子：
--
作者：
Zhanwen Han;P. Podsiadlowski;A. Lynas-Gray;K. Schawinski
通讯作者：
Zhanwen Han;P. Podsiadlowski;A. Lynas-Gray;K. Schawinski