On the size of convective cores in rotating, upper main-sequence stars

Details On the size of convective cores in rotating, upper main-sequence stars On the size of convective cores in rotating, upper main-sequence stars

Nov 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...310..273m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 310, Nov. 1, 1986, p. 273-276.

Statistics

Computation

8

Main Sequence Stars, Size (Dimensions), Stellar Cores, Stellar Rotation, Convective Heat Transfer, Stellar Luminosity, Stellar Models

Scientific paper

The effects of rotation on the structure of upper main sequence stars are reviewed, and the effects resulting from alterations of the convective-radiative stability criterion due to changes in the radiative gradient are explicitly modeled and analyzed. It is found that rotation leads to a smaller convective core and reduced luminosity, the coupled effects of which lead to little change in the main sequence lifetime. It is noted that the rotational modification to the Schwarzschild criterion suggested by Sreenivasan and Wilson (1985) has in fact been included in the computations conducted by previous authors.

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