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Proof Delivery Form Proceedings of the International Astronomical Union Date of delivery : 5 May 2016

Here, we present a set of time-dependent 3D RMHD simulations of a M-dwarf star 9 representative of AD Leo, which extend from the upper convection zone into the chromosphere. 10 The 3D model atmospheres are characterized by a very dynamic and intermittent structure on 11 small spatial and temporal scales and a wealth of physical processes, which by nature cannot 12 be described by means of 1D static model atmospheres. Artificial observations of these models 13 imply that a combination of complementary diagnostics such as Ca II lines and the continuum 14 intensity from UV to millimeter wavelengths, probe various properties of the dynamics, thermal 15 and magnetic structure of the photosphere and the chromosphere and thus provide measures of 16 stellar activity, which can be compared to observations. The complicated magnetic field structure 17 and its imprint in synthetic diagnostics may have important implications for the understanding 18 and characterization of stellar activity and with it possibly for the evaluation of planetary 19 habitability around active M-dwarf stars. 20