http://arxiv.org/abs/1401.5511
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 $10^{-9}\,\text{M}_\odot\,\text{year}^{-1}$, while for the cooler ones the mass-loss rate is by more than three orders of magnitude lower. Main sequence B stars with solar abundance and effective temperatures lower than about $15\,000\,\text{K}$ (later than the 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 modified abundance of heavier elements to study the winds of chemically peculiar stars. The mass-loss rate may both 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 $15\,000\,\text{K}$. The winds of main-sequence B stars lie below the static limit, i.e., a static atmosphere solution is also possible. This points to an important problem of initiation of these winds. We discuss the implications of our models for the rotational braking, filling the magnetosphere of Bp stars and for chemically peculiar stars.
Thu, 23 Jan 14
48/70
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