Sign on
ADS Classic is now deprecated. It will be completely retired in October 2019. This page will automatically redirect to the new ADS interface at that point.

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic On-line Article (HTML)
· Table of Contents
· References in the Article
· Reads History
· Translate This Page
Variation in convective properties across the HR diagram
Tanner, Joel; Basu, Sarbani; Demarque, Pierre; Robinson, Frank
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)
Astrophysical Dynamics: From Stars to Galaxies, Proceedings of the International Astronomical Union, IAU Symposium, Volume 271, p. 401-402
Publication Date:
stars: atmospheres, stars: evolution
Abstract Copyright:
(c) 2011: Copyright © International Astronomical Union 2011
Bibliographic Code:


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.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

Find Similar Abstracts:

Use: Authors
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
arXiv e-prints