Abstract
The rotation of post-Z.A.M.S. cool-stars is reviewed. Once off the main sequence, cool stars seem to shift from internal uniform to differential rotation. Intermediate mass stars may encounter a “rotational boundary,” which collapses their surface rotations to a quasi-δ-function thereafter. This boundary occurs at ~G5111 and may extend down to the late-F-dwarfs. If so, the rotation of solar-type dwarfs could be controlled between narrow limits by a “rotostat”.
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Smith, M.A. (1987). Post-zero-age main sequence rotation among late-type stars. In: Linsky, J.L., Stencel, R.E. (eds) Cool Stars, Stellar Systems, and the Sun. Lecture Notes in Physics, vol 291. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-18653-0_133
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DOI: https://doi.org/10.1007/3-540-18653-0_133
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