The size of convective cores in rotating stellar models

Details The size of convective cores in rotating stellar models The size of convective cores in rotating stellar models

Jun 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...341..939s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 341, June 15, 1989, p. 939-947. Research supported by NSERC.

Statistics

Computation

7

Astronomical Models, Computational Astrophysics, Stellar Cores, Stellar Rotation, Adiabatic Conditions, Stellar Envelopes, Stellar Evolution, Stellar Mass, Stellar Radiation

Scientific paper

It is argued that convective cores of differentially rotating stellar models conserving specific angular momentum should be larger by comparing the adiabatic and radiative gradients of rotating models with those of nonrotating models. It is shown that the reverse follows from models with rigid rotation as long as the ratio of the centrifugal force to gravity, Lambda, is small. It is also shown that Lambda increases over sevenfold between the surface and the core when its surface value, Lambda(s), is barely above 1 percent. Realistic studies of rotating models would therefore have to be at least two-dimensional when Lambda(s) exceeds about 20 percent and mass loss and other concomitant effects are included.

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