Stellar evolution with rotation
III. Meridional circulation with µ-gradients and non-stationarity
Received 4 October 1997 / Accepted 18 March 1998
Models of stellar evolution with rotation are very much needed in order to interpret recent stellar properties, in particular for massive stars. For that we proceed to a detailed investigation of some critical physical processes in rotating stars:
1. The equation expressing the transport of angular momentum by circulation and diffusion is revised to also account for expansion and contraction in non-stationary models.
2. We examine the current expressions for the velocity of the meridional circulation, also taking into account µ-gradients and horizontal turbulence. We show that there are no "µ-currents" but just meridional currents which can be sizeably influenced by the gradients of mean molecular weight µ. A proper account of the µ-gradients may reduce by one or two orders of magnitude with respect to current expressions.
3. While the usual expressions for the meridional circulation would predict an infinite velocity at the edge of a radiative and semiconvective zone and an inverted circulation in a semiconvective zone, the present developments give a continuity of the solutions for the circulation.
4. The approximation of a stationary circulation, which is no longer valid after the main-sequence phase, is also removed and the case of a general equation of state is considered. We notice that in the stationary regime the horizontal fluctuations of µ represent some fixed fraction of the vertical µ-gradient. To first order, this fraction is not dependent on rotation, because the building of horizontal fluctuations by the circulation is compensated by the smoothing due to horizontal turbulence.
Key words: stars: rotation stars: early-type stars: interior
© European Southern Observatory (ESO) 1998
Online publication: June 2, 1998