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Title:
Variation in convective properties across the HR diagram
Authors:
Tanner, Joel; Basu, Sarbani; Demarque, Pierre; Robinson, Frank
Affiliation:
AA(Yale University, New Haven, Connecticut, USA), AB(Yale University, New Haven, Connecticut, USA), AC(Yale University, New Haven, Connecticut, USA), AD(Yale University, New Haven, Connecticut, USA)
Publication:
Astrophysical Dynamics: From Stars to Galaxies, Proceedings of the International Astronomical Union, IAU Symposium, Volume 271, p. 401-402
Publication Date:
08/2011
Origin:
CUP
Keywords:
stars: atmospheres, stars: evolution
Abstract Copyright:
(c) 2011: Copyright © International Astronomical Union 2011
DOI:
10.1017/S1743921311017996
Bibliographic Code:
2011IAUS..271..401T

Abstract

We perform 3D radiative hydrodynamic simulations to study convection in low-mass main-sequence stars with the aim of improving stellar models. Comparing models from a 0.90 Msolar evolutionary track with 3D simulations reveals distinct differences between simulations and mixing length theory. The simulations show obvious structural differences throughout the superadiabatic layer where convection is inefficient at transporting energy. The discrepancy between MLT and simulation changes as the star evolves and the dynamical effects of turbulence increase. Further, the simulations reveal a T-tau relation that is sensitive to the strength of the turbulence, which is in contrast to 1D stellar models that use the same T-tau relation across the HR diagram.
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