Turbulent Convection in Stars: Some Recent Advances

Details Turbulent Convection in Stars: Some Recent Advances Turbulent Convection in Stars: Some Recent Advances

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aspc..374...27d&link_type=abstract

From Stars to Galaxies: Building the Pieces to Build Up the Universe. ASP Conference Series, Vol. 374, proceedings of the confer

Physics

1

Scientific paper

Advances are discussed in two areas in which improved numerical treatments of radiation hydrodynamics, coupled with advances in helio- and asteroseismology, provide stringent tests of stellar interior models. Stellar evolution data are fundamental building blocks in population studies. The first area is convective core overshoot which affects evolutionary timescales and the evolution of integrated spectral energy distributions in stellar systems. The second area is the treatment of radiation hydrodynamics in the outer layers of cool stars with convection zones, with the aim of removing the shortcomings of the canonical mixing-length theory. A realistic physical description is also needed to calculate p-mode excitation and amplitudes, tidal dissipation in convection zones, and to derive accurate chemical abundances.

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