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.
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