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K. L. Chan (The Hong Kong University of Science and Technology)
Differential rotation is responsible for a number of important phenomena (e.g. magnetic cycle, spots) associated with cool stars. It has generally been accepted that convection plays a key role in the generation of differential rotation, but the mechanism has not been worked out from first principles. Numerical modeling offers most promises but the approach is plagued by hidden pitfalls. We are going to discuss our new attempt to study differential rotation with a global numerical model, where and how to avoid the common pitfalls, and the encouraging case that shows similarity with the solar angular velocity distribution.
This research is supported by the Research Grant Council of Hong Kong.
The author(s) of this abstract have provided an email address for comments about the abstract: maklchan@ust.hk