The stellar luminosity and depth of the convective envelope vary rapidly with mass for G- and K-type main sequence stars .
In order to understand how these properties influence the convective turbulence , differential rotation , and meridional circulation , we have carried out 3D dynamical simulations of the interiors of rotating main sequence stars , using the anelastic spherical harmonic ( ASH ) code .
The stars in our simulations have masses of 0.5 , 0.7 , 0.9 , and 1.1 M _ { \odot } , corresponding to spectral types K7 through G0 , and rotate at the same angular speed as the sun .
We identify several trends of convection zone properties with stellar mass , exhibited by the simulations .
The convective velocities , temperature contrast between up- and downflows , and meridional circulation velocities all increase with stellar luminosity .
As a consequence of the trend in convective velocity , the Rossby number ( at a fixed rotation rate ) increases and the convective turnover timescales decrease significantly with increasing stellar mass .
The 3 lowest mass cases exhibit solar-like differential rotation , in a sense that they show a maximum rotation at the equator and minimum at higher latitudes , but the 1.1 M _ { \odot } case exhibits anti-solar rotation .
At low mass , the meridional circulation is multi-cellular and aligned with the rotation axis ; as the mass increases , the circulation pattern tends toward a unicellular structure covering each hemisphere in the convection zone .