Magnetic Field Generation in Fully Convective Rotating Spheres

Magnetohydrodynamic simulations of fully convective, rotating spheres with volume heating near the center and cooling at the surface are presented. The dynamo-generated magnetic field saturates at equipartition field strength near the surface. In the interior, the field is dominated by small-scale structures, but outside the sphere by the global scale. Azimuthal averages of the field reveal a large-scale field of smaller amplitude also inside the star. The internal angular velocity shows some tendency to be constant along cylinders and is “anti-solar” (fastest at the poles and slowest at the equator). Subject headings: stars: low-mass, stars: pre-main sequence, stars: magnetic fields, MHD, convection, turbulence