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Some of the quiet solar magnetic flux could be attributed to a small-scaledynamo (SSD) operating in the convection zone. An SSD operating in coolmain-sequence stars is expected to affect the atmospheric structure, inparticular the convection, and should have observational signatures. We aim toinvestigate the distribution of these fields as well as their effect onintensity characteristics, velocities and spatial distribution of kinetic (KE)and magnetic energy (ME) in the lower photosphere of spectral types F3V, G2V,K0V and M0V using 3D radiative-MHD simulations. PDFs of field strength at the$\tau=1$ surface are quite similar for all cases. The M0V star displays thestrongest fields, but relative to the gas pressure, the fields on the F3V starreach the largest values. All stars display an excess of horizontal fieldrelative to vertical field in the middle photosphere, with this excess becomingincreasingly prominent towards later spectral types. These fields result in adecrease in upflow velocities, slightly smaller granules as well as theformation of bright points in intergranular lanes. The spatial distribution ofKE and ME is also similar for all cases, implying a simple pressure scaleheight proportionality of important scales. SSD fields have rather similareffects on the photospheres of cool main-sequence stars, namely, a significantreduction in convective velocities as well as a slight reduction in granulesize, and concentration of field to kG levels in intergranular lanes associatedwith the formation of bright points. The distribution of field strengths andenergies is also rather similar.

Small-scale Dynamo in Cool Stars III. Changes in the photospheres of F3V to M0V stars