Improved solar models constructed with a formulation of convection for stellar structure and evolution calculations without the mixing-length theory approximations

Details Improved solar models constructed with a formulation of convection for stellar structure and evolution calculations without the mixing-length theory approximations Improved solar models constructed with a formulation of convection for stellar structure and evolution calculations without the mixing-length theory approximations

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...403l..79l&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 403, no. 2, p. L79-L82.

Astronomy and Astrophysics

Astrophysics

15

Mixing Length Flow Theory, Stellar Convection, Stellar Evolution, Stellar Models, Stellar Structure, Kinetic Energy, Stellar Interiors

Scientific paper

We have updated a previous attempt to incorporate within a solar model a treatment of convection based upon numerical simulations of convection rather than mixing-length theory (MLT). We have modified our formulation of convection for a better treatment of the kinetic energy flux. Our solar model has been updated to include a complete range of OPAL opacities, the Debye-Hueckel correction to the equation of state, helium diffusion due to gravitational settling, and atmospheres by Kurucz. We construct a series of models using both MLT and our revised formulation of convection and the compared results to measurements of the solar radius, the solar luminosity, and the depth of the solar convection zone as inferred from helioseismology. We find X(solar) = 0.702 +/- 0.005, Y(solar) = 0.278 +/- 0.005, and Z(solar) = 0.0193 +/- 0.0005.

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