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Magnetic activity is a ubiquitous feature of stars with convective outerlayers, with implications from stellar evolution to planetary atmospheres.Investigating the mechanisms responsible for the observed stellar activitysignals from days to billions of years is important in deepening ourunderstanding of the spatial configurations and temporal patterns of stellardynamos, including that of the Sun. In this paper, we focus on three problemsand their possible solutions. We start with direct field measurements and showhow they probe the dependence of magnetic flux and its density on stellarproperties and activity indicators. Next, we review the currentstate-of-the-art in physics-based models of photospheric activity patterns andtheir variation from rotational to activity-cycle timescales. We then outlinethe current state of understanding in the long-term evolution of stellardynamos, first by using chromospheric and coronal activity diagnostics, thenwith model-based implications on magnetic braking, which is the key mechanismby which stars spin down and become inactive as they age. We conclude bydiscussing possible directions to improve the modeling and analysis of stellarmagnetic fields.

Scaling and Evolution of Stellar Magnetic Activity