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The convective envelopes of cool main-sequence stars harbour magnetic fieldswith a complex global and local structure. These fields affect the near-surfaceconvection and the outer stellar atmospheres in many ways and are responsiblefor the observable magnetic activity of stars. Our aim is to understand thelocal structure in unipolar regions with moderate average magnetic fluxdensity. These correspond to plage regions covering a substantial fraction ofthe surface of the Sun (and likely also the surface of other Sun-like stars)during periods of high magnetic activity. We analyse the results of 18local-box magnetohydrodynamics simulations covering the upper layers of theconvection zones and the photospheres of cool main-sequence stars of spectraltypes F to early M. The average vertical field in these simulations ranges from20 to 500G. We find a substantial variation of the properties of the surfacemagnetoconvection between main-sequence stars of different spectral types. As aconsequence of a reduced efficiency of the convective collapse of flux tubes, Mdwarfs lack bright magnetic structures in unipolar regions of moderate fieldstrength. The spatial correlation between velocity and the magnetic field aswell as the lifetime of magnetic structures and their sizes relative to thegranules vary significantly along the model sequence of stellar types.

Three-dimensional simulations of near-surface convection in main-sequence stars. III. The structure of small-scale magnetic flux concentrations