By the action of turbulence the convection zone of the Sun rotates
differentially, i.e. with nonuniform angular velocity. After explaining the
observed solar rotation law by
our numerical models , we can now make
predictions about the rotation laws inside other stars.
Moreover, we can judge the theory's reliability after including
new stellar data.
Global acoustic oscillations of the Sun, used by helioseismology to probe the
solar interior, are excited by turbulence in the convection zone - and also
destructed by the same turbulence. Scrutinized analysis of the
oscillation spectrum provides us with the properties of the
otherwise unobservable turbulence.
It is of key importance in modern astrophysics to have a profound understanding
of the solar magnetic field. The well-known 22-year solar
cycle of the magnetic
field results from an interplay of turbulence, gravitation and
rotation. State-of-the-art models (in the
`overshoot'-region) are able to explain most of the
properties of the solar cycle.
