MHD disc winds
arXiv:astro-ph/0607216 · doi:10.1007/978-3-540-68035-2_8
Abstract
This is a doctorate level lecture on the physics of accretion discs driving magnetically self-confined jets, usually referred to in the literature as disc winds. I will first review the governing magnetohydrodynamic equations and then discuss their physical content. At that level, necessary conditions to drive jets from keplerian accretion discs can already be derived. These conditions are validated with self-similar calculations of accretion-ejection structures. In a second part, I will critically discuss the biases introduced when using self-similarity as well as some other questions such as: Are these systems really unstable? Can a standard accretion disc provide the conditions to launch jets in its innermost parts? What is the difference between X-winds and disc-winds? Finally, the magnetic interaction between a protostar and its circumstellar disc will be discussed with a focus on stellar spin down.
25 pages, 11 figures to be published in Lecture Notes in Physics, "Jets from Young Stars: Models and Constraints", J. Ferreira, C. Dougados and E. Whelan (eds), Springer Verlag
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