Recent advances in spectropolarimetry have shown that stars arrive on the main sequence with a wide range of coronal magnetic geometries. From 15 solar mass stars with radiative interiors down to very low mass stars of a few tenths of a solar mass, differences in a stellar internal structure appear to lead to very different magnetic fields. For very young stars, this is particularly important as their internal structure may change as they age. This has implications not only for the stellar X-ray and radio emission, but also for stellar spin down, photometric variability produced by starspots and the nature of the interaction between stars and their planets. In this talk I will review these recent changes in our understanding of stellar coronae.

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