Rotation and Stellar Evolution

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Abstract
Sweet's discussion (1) of rotational currents in a Cowling model star is reviewed. It is shown that the non-spherical distribution of matter set up by the currents themselves tends to choke back the motion, so that no rotationally stable star can suffer any considerable mixing between core and envelope, if the angular velocity is nearly constant throughout the star. If, however, the rotation rate increases substantially inwards, enough mixing can occur to influence seriously the evolution of the star.

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