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‘Negative’ surface differential rotation in stars having low Coriolis numbers (slow rotation or high turbulence)

Published online by Cambridge University Press:  26 February 2010

Kwing L. Chan
Kwing L. Chan*
Affiliation:
Department of Mathematics, Hong Kong University of Science and Technology, Hong Kong, China email: maklchan@ust.hk
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Abstract

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A general picture of differential rotation in cool stars is that they are ‘solar-like’, with the equator spinning faster than the poles. Such surface differential rotation profiles have also been demonstrated by some three-dimensional simulations. In our numerical investigation of rotating convection (both regional and global), we found that this picture is not universally applicable. The equator may spin substantially slower than the poles (Ωequator − Ωpole)/Ω can reach −50%). The key parameter that determines the transition in behavior is the Coriolis number (inverse Rossby number). ‘Negative’ differential rotation of the equator (relative to the mean rotation) occurs if the Coriolis number is below a critical value.

Keywords

stars: interiorsrotationconvection
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S264: Solar and Stellar Variability: Impact on Earth and Planets , August 2009 , pp. 219 - 221
Copyright
Copyright © International Astronomical Union 2010

References

Chan, K. L. 2003, in Turcotte, S., Keller, S. C. & Cavallo, M. (eds.), 3D Stellar Evolution (Ann Arbor: Sheridan), p. 168 (can be found at http://www.math.ust.hk/~maklchan)Google Scholar
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