Previous abstract Next abstract The vigorous turbulence that
results from convective instability within rotating stars serves
to not only transport heat but also redistribute angular
momentum and chemical species, and can yield magnetic dynamo
action. A hallmark of such turbulence constrained by rotation
and stratification is that large-scale coherent structures and
strong mean flows can coexist with the intense smaller-scale
turbulence. Helioseismology is suggesting that the resulting
differential rotation within the convection zone of a star like
the sun yields serious puzzles about the interaction of
convection and rotation. Understanding such nonlinear dynamics
at a fundamental level raises formidable challenges because of
the broad range of scales of motion that must be resolved. High-
performance computing offers the opportunity to make substantial
inroads in studying the properties of such astrophysical
turbulence. An interdisciplinary team of researchers at several
institutions is working jointly on pr