Magnetic activity in low-mass stars: Do the brakes come off?

Details Magnetic activity in low-mass stars: Do the brakes come off? Magnetic activity in low-mass stars: Do the brakes come off?

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aspc..261...11c&link_type=abstract

The Physics of Cataclysmic Variables and Related Objects, ASP Conference Proceedings, Vol. 261. Edited by B. T. Gänsicke, K. Beu

Physics

8

Scientific paper

Dynamo-driven magnetic activity is ubiquitous among rotating stars with outer convective zones, and the secondary stars of CV systems should be no exception. Angular momentum loss via a magnetically-driven wind originating from the secondary is thought to be of crucial importance in CV evolution, and magnetic fields on the secondary may have some influence on the rate of mass transfer through the L1 point. Stellar surface imaging methods and large-scale rotation and activity surveys in open clusters over the last few years have greatly improved our knowledge of magnetic field generation and braking behaviour in single low-mass stars. In this paper I review our current state of knowledge concerning magnetic braking and its relevance to long-held ideas about CV evolution and the origin of the period gap, and speculate on what might be achieved by applying stellar surface imaging codes to CVs and single fully-convective dwarfs in the 8-metre telescope era.

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