The prediction of stellar effective temperatures from the mixing-length theory of convection

Details The prediction of stellar effective temperatures from the mixing-length theory of convection The prediction of stellar effective temperatures from the mixing-length theory of convection

Mar 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...352..279p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 352, March 20, 1990, p. 279-290. Research supported by NSERC.

Astronomy and Astrophysics

Astrophysics

29

Convection, Cool Stars, Mixing Length Flow Theory, Stellar Atmospheres, Stellar Temperature, Astronomical Models, Main Sequence Stars, Photosphere, Stellar Evolution, Stellar Interiors, Stellar Radiation

Scientific paper

A generalized version of the mixing-length theory (MLT) of convection, along with simplifications in the limits of high and low convective efficiency, is described. This forms the basis for a study of the effects of proposed modifications to the original (Boehm-Vitense, 1958) form of the MLT on the predicted effective temperatures of cool stars. These modifications include the parameters y and m. It is found that none of the suggested refinements to the MLT affect the location and shape of an evolutionary track on the H-R diagram in ways that cannot be mimicked to high accuracy by a suitable choice of mixing length parameters alone. Thus, if mixing length parameters is calibrated by comparing stellar models with observed main-sequence stars with well-determined properties, then the subsequent evolutionary tracks and isochrones are uniquely defined, regardless of what version of the MLT is used in the calculations. A careful examination of the Revised Yale Isochrones suggests that the Teff scale of these isochrones is inconsistent with the assumed MLT, thereby resolving much of the known discrepancies between these calculations and those of VandenBerg and Bell (1958).

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