Simulations of facular magnetic fields on cool stars - I. Main-sequence stars with solar metallicity

Open Access

Fig. 6

Changes in square of vertical velocity, $v_{z}^{2}$ $Mathematical equation: $\[v_{z}^{2}\]$$ (top), and in the ratio of horizontal to vertical velocities, v_h,rms/v_z,rms (bottom), for the 300 G case relative to the SSD case for all four stellar types.

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