Abstract
All main sequence stars lose mass via stellar winds. The winds of cool stars like the sun are driven by gas pressure gradient. However, the winds of hot massive stars which tend to be luminous are driven by emitted by the star radiation pressure. Mass loss from such winds are significantly higher. In this article, I describe the nature of such radiatively driven winds and show how they interact with rotation and magnetic fields leading to stellar spindown and large-scale disk-like structures. In particular, I show that the overall degree to which the wind is influenced by the field depends largely on a single, dimensionless, “wind magnetic confinement parameter”, η ∗ \(({=} B_{\mathrm{eq}}^{2} R_{\ast}^{2}/{\dot{M}} v_{\infty})\), which characterizes the ratio between magnetic field energy density and kinetic energy density of the wind.
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Notes
- 1.
This is closely related to the commonly used rotation parameter ω≡Ω/Ω crit, defined by the star’s angular rotating frequency Ω relative to the value this would have as the star approaches “critical” rotation, Ω c . The choice here more directly relates to the additional local speed needed to propel material into Keplerian orbit, and avoids some subtle assumptions (e.g. rigid-body rotation using a Roche potential for gravity) about how the global stellar envelope structure adjusts to approaching the critical rotation limit.
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Acknowledgements
The author thanks CNRS for the invitation to the school devoted on the topic “From solar environment to stellar environment” held in Roscoff (F).
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ud-Doula, A. (2013). Stellar Winds, Magnetic Fields and Disks. In: Rozelot, JP., Neiner, C. (eds) The Environments of the Sun and the Stars. Lecture Notes in Physics, vol 857. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-30648-8_8
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