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The surface rotation rates of young solar-type stars vary rapidly with agefrom the end of the pre-main sequence through the early main sequence.Important changes in the dynamos operating in these stars may result from thisevolution, which should be observable in their surface magnetic fields. Here wepresent a study aimed at observing the evolution of these magnetic fieldsthrough this critical time period. We observed stars in open clusters andstellar associations of known ages, and used Zeeman Doppler Imaging tocharacterize their complex magnetic large-scale fields. Presented here areresults for 15 stars, from 5 associations, with ages from 20 to 250 Myr, massesfrom 0.7 to 1.2 solar masses, and rotation periods from 0.4 to 6 days. We findcomplex large-scale magnetic field geometries, with global average strengthsfrom 14 to 140 G. There is a clear trend towards decreasing average large-scalemagnetic field strength with age, and a tight correlation between magneticfield strength and Rossby number. Comparing the magnetic properties of ourzero-age main sequence sample to those of both younger and older stars, itappears that the magnetic evolution of solar-type stars during the pre-mainsequence is primarily driven by structural changes, while it closely followsthe stars' rotational evolution on the main sequence.

The evolution of surface magnetic fields in young solar-type stars I: the first 250 Myr