Volume 459, Number 2, November IV 2006
|Page(s)||599 - 612|
|Published online||12 September 2006|
Energy transport, overshoot, and mixing in the atmospheres of M-type main- and pre-main-sequence objects
GEPI, CIFIST, Observatoire de Paris-Meudon, 5 place Jules Janssen, 92195 Meudon Cedex, France e-mail: Hans.Ludwig@obspm.fr
2 Lund Observatory, Lund University, Box 43, 22100 Lund, Sweden
3 École Normale Supérieure de Lyon, Centre de Recherche Astronomique de Lyon, 46 allée d'Italie, 69364 Lyon Cedex 07, France; CNRS, UMR 5574; Université de Lyon 1, Lyon, France
4 Institut d'Astrophysique de Paris, CNRS, UMR 7095, 98bis boulevard Arago, 75014 Paris, France; Université Pierre et Marie Curie-Paris 6, 75005 Paris, France
5 Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany
Accepted: 9 August 2006
We constructed hydrodynamical model atmospheres for mid M-type main-, as well as pre-main-sequence (PMS) objects. Despite the complex chemistry encountered in these cool atmospheres a reasonably accurate representation of the radiative transfer is possible, even in the context of time-dependent and three-dimensional models. The models provide detailed information about the morphology of M-type granulation and statistical properties of the convective surface flows. In particular, we determined the efficiency of the convective energy transport, and the efficiency of mixing by convective overshoot. The convective transport efficiency was expressed in terms of an equivalent mixing-length parameter in the formulation of mixing-length theory (MLT) given by Mihalas (1978). amounts to values around ≈2 for matching the entropy of the deep, adiabatically stratified regions of the convective envelope, and lies between 2.5 and 3.0 for matching the thermal structure of the deep photosphere. For current spectral analysis of PMS objects this implies that MLT models based on overestimate the effective temperature by 100 K and surface gravities by 0.25 dex. The average thermal structure of the formally convectively stable layers is little affected by convective overshoot and wave heating, i.e., stays close to radiative equilibrium conditions. Our models suggest that the rate of mixing by convective overshoot declines exponentially with geometrical distance to the Schwarzschild stability boundary. It increases at given effective temperature with decreasing gravitational acceleration.
Key words: convection / hydrodynamics / radiative transfer / stars: atmospheres / stars: late-type
© ESO, 2006
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