Abstract
The accumulating observational data point clearly to a basic picture of stellar activity dominated by magnetic fields maintained by dynamo action, dependent on the star’s rotation. There is some tentative evidence that in the pre-main sequence phase there is also some primeval magnetic flux, which may be dynamically significant for the T Tauri phenomenon. Possible helioseismological constraints on any such relic flux in the solar core are analysed. A simple model for the external magnetic field has both a wind zone and a corotating dead zone; the predicted rotational history of the star is discussed, and some support for the model noted from observations of a young, rapidly rotating dwarf star. Some of the impressive achievements of current dynamo theory are summarised. Continual interactions between observers and theoretical workers on dynamos and stellar magnetospheres offer the best hope for rapid advances in the near future.
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Mestel, L. (1988). Stellar Magnetic Fields, Origin and Structure. In: Havnes, O., Pettersen, B.R., Schmitt, J.H.M.M., Solheim, J.E. (eds) Activity in Cool Star Envelopes. Astrophysics and Space Science Library, vol 143. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-2951-7_1
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DOI: https://doi.org/10.1007/978-94-009-2951-7_1
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