Abstract
In this paper we review the principal elements of the Yale code for evolving rotating stars (YREC). The various mechanisms to distribute angular momentum in the solar interior used in the code are discussed, both in regard to their properties and their consequences in the stellar models. In particular, two general types of mechanisms exist, one which depends on the velocity of rotation, and the other which depends on the radial gradient of this quantity. The regions where these mechanisms operate effectively, and the times when this occurs, and possibly the efficiency of these transfer mechanisms to cause material mixing, depend on which of the two types they belong.
The main effects of rotation in stellar evolution are on the surface velocity and the surface abundance of trace elements and CNO as a function of time. The effects on the internal structure, and therefore the evolution, as shown in an H-R diagram, are much smaller. Because of the structure differences in stars of different composition, the consequences also differ with population type.
We have computed stellar models including the effects of rotation for the Sun, open cluster stars, and halo stars. Solar-calibrated models with rotationally-induced mixing can reproduce the main features of the surface lithium depletion pattern and surface velocity both as a function of stellar mass within an open cluster and as a function of time from cluster to cluster, and also in halo dwarfs. Furthermore, our halo star models have substantial differential rotation with depth. This differential rotation provides them with enough internal angular momentum to explain the high observed rotation velocities of evolved metal-poor horizontal branch stars, while at the same time they rotate slowly enough at the surface to be consistent with the low upper limits on the rotation of metal-poor main sequence stars. By contrast, models constructed assuming rigid rotation in the main sequence cannot reconcile the high rotation velocities of evolved stars with the low rotation velocities of their main sequence progenitors.
The solar models constructed in this fashion show that the present Sun rotates with increasing angular velocity in the deep interior.
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Sofia, S., Pinsonneault, M., Deliyannis, C.P. (1991). Evolutionary Models of Rotating Stars. In: Catalano, S., Stauffer, J.R. (eds) Angular Momentum Evolution of Young Stars. NATO ASI Series, vol 340. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-3580-1_30
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DOI: https://doi.org/10.1007/978-94-011-3580-1_30
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