Mass loss in main-sequence B stars
Mass loss in main-sequence B stars
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DOI：
10.1051/0004-6361/201321980
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发表时间：
2014-01
影响因子：
6.5
通讯作者：
J. Krtička
中科院分区：
文献类型：
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作者：
J. Krtička
我们计算了主序B星的辐射驱动风模式，并给出了风的质量损失率和终端速度。主序的质量损失率很大程度上取决于恒星的有效温度。对于最热的B星，质量损失率达到1 -9个月/年，而对于较冷的B星，质量损失率要低3个数量级以上。太阳丰度和有效温度低于15000 K（晚于光谱型B5）的主序B恒星没有任何均匀的线驱动风。我们预测太阳化学成分的风质量损失率和重元素的修改丰度，以研究化学特殊恒星的风。质量损失率可能随着丰度的增加而增加或减少，这取决于诱导涌现通量重新分布的重要性。硅含量过高的恒星可能有均匀的风，甚至低于太阳丰度风的极限15000k。主序B星的风位于静态极限以下，也就是说，静态大气的解决方案也是可能的。这指出了一个关于这些风的起源的重要问题。我们讨论了我们的模型对旋转制动的影响，填充Bp恒星的磁层，以及化学上特殊的恒星。
We calculate radiatively driven wind models of main-sequence B stars and provide the wind mass-loss rates and terminal velocities. The main-sequence mass-loss rate strongly depends on the stellar effective temperature. For the hottest B stars the mass-loss rate amounts to 1d-9 Mo/year, while for the cooler ones the mass-loss rate is lower by more than three orders of magnitude. Main-sequence B stars with solar abundance and effective temperatures lower than about 15000 K (later than spectral type B5) do not have any homogeneous line-driven wind. We predict the wind mass-loss rates for the solar chemical composition and for the modified abundance of heavier elements to study the winds of chemically peculiar stars. The mass-loss rate may either increase or decrease with increasing abundance, depending on the importance of the induced emergent flux redistribution. Stars with overabundant silicon may have homogeneous winds even below the solar abundance wind limit at 15000 K. The winds of main-sequence B stars lie below the static limit, that is, a static atmosphere solution is also possible. This points to an important problem regarding the initiation of these winds. We discuss the implications of our models for rotational braking, filling the magnetosphere of Bp stars, and for chemically peculiar stars.