Abstract
It is generally accepted that magnetic fields in late-type stars are produced by dynamo action in their convection zones. In this review I shall discuss the impact on dynamo models of the observations that have been described by Pallavicini, Byrne and Giampapa et al. in these Proceedings. The magnetic behaviour of these stars is governed by a few control parameters: the mass and composition determine stellar structure and, in particular, the depth of the convection zone, while the rotation rate, Ω, controls the degree of magnetic activity, which in turn affects magnetic braking. I shall focus on G-stars like the Sun, whose rotational history is well established.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
