Stars with convective envelopes can generate strong magnetic fields through rotationally driven dynamos. Theory suggests that the maximum magnetic field strength depends on the energy budget stored in the stellar convective shell and can reach values of several kilogauss in fastest rotating stars. We test this predictions by measuring total magnetic flux and polarization in a sample of sun-like stars that rotate close to the activity saturation limit. We detect average magnetic flux densities of several hundred G in several of our targets, with the strongest field of about 1~kG in a K type star V383~Lac showing that young sun-like stars can produce average fields on the kG level.

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poster #142