Stellar Winds, Magnetic Fields and Disks View Full Text


Ontology type: schema:Chapter     


Chapter Info

DATE

2013

AUTHORS

Asif ud-Doula

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. More... »

PAGES

207-230

Book

TITLE

The Environments of the Sun and the Stars

ISBN

978-3-642-30647-1
978-3-642-30648-8

Author Affiliations

Identifiers

URI

http://scigraph.springernature.com/pub.10.1007/978-3-642-30648-8_8

DOI

http://dx.doi.org/10.1007/978-3-642-30648-8_8

DIMENSIONS

https://app.dimensions.ai/details/publication/pub.1015781193


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