Hostname: page-component-848d4c4894-p2v8j Total loading time: 0.001 Render date: 2024-05-24T13:54:41.558Z Has data issue: false hasContentIssue false

‘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*
Affiliation:
Department of Mathematics, Hong Kong University of Science and Technology, Hong Kong, China email: maklchan@ust.hk
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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.

Type
Contributed Papers
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
Chan, K. L., Mayr, H. G., Mengel, J. G., & Harris, I. 1994, J. Comput. Phys., 113, 165CrossRefGoogle Scholar
Erdem, A. et al. 2009, New Astron., 14, 545CrossRefGoogle Scholar
Kitchatinov, L. L. & Rudiger, G. 2004, AN, 325, 496Google Scholar
Palacios, A. & Brun, A. S. 2007, AN, 328, 1114Google Scholar
Steffen, M. & Freytag, B. 2007, AN, 328, 1054Google Scholar