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Variation in convective properties across the HR diagram

Published online by Cambridge University Press:  12 August 2011

Joel Tanner ,
Sarbani Basu ,
Pierre Demarque  and
Frank Robinson
Joel Tanner
Affiliation:
Yale University, New Haven, Connecticut, USA
Sarbani Basu
Affiliation:
Yale University, New Haven, Connecticut, USA
Pierre Demarque
Affiliation:
Yale University, New Haven, Connecticut, USA
Frank Robinson
Affiliation:
Yale University, New Haven, Connecticut, USA
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Abstract

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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 M⊙ 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.

Keywords

stars: atmospheresstars: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S271: Astrophysical Dynamics: From Stars to Galaxies , June 2010 , pp. 401 - 402
Copyright
Copyright © International Astronomical Union 2011

References

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