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Linking 1D Stellar Evolution to 3D Hydrodynamic Simulations

Published online by Cambridge University Press:  23 January 2015

A. Cristini ,
R. Hirschi ,
C. Georgy ,
C. Meakin ,
D. Arnett  and
M. Viallet
A. Cristini
Affiliation:
Astrophysics group, Keele University, Lennard-Jones Building, Keele, ST5 5BG, UK email: [email protected]
R. Hirschi
Affiliation:
Astrophysics group, Keele University, Lennard-Jones Building, Keele, ST5 5BG, UK email: [email protected] Kavli IPMU (WPI), The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
C. Georgy
Affiliation:
Astrophysics group, Keele University, Lennard-Jones Building, Keele, ST5 5BG, UK email: [email protected]
C. Meakin
Affiliation:
Department of Astronomy, University of Arizona, Tucson, AZ 85721, USA
D. Arnett
Affiliation:
Department of Astronomy, University of Arizona, Tucson, AZ 85721, USA
M. Viallet
Affiliation:
Max-Planck-Institut für Astrophysik, Garching, D-85741, Germany
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Abstract

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In this contribution we present initial results of a study on convective boundary mixing (CBM) in massive stellar models using the GENEVA stellar evolution code (Eggenberger et al.2008). Before undertaking costly 3D hydrodynamic simulations, it is important to study the general properties of convective boundaries, such as the: composition jump; pressure gradient; and “stiffness”. Models for a 15M⊙ star were computed. We found that for convective shells above the core, the lower (in radius or mass) boundaries are “stiffer” according to the bulk Richardson number than the relative upper (Schwarzschild) boundaries. Thus, we expect reduced CBM at the lower boundaries in comparison to the upper. This has implications on flame front propagation and the onset of novae.

Keywords

convectionhydrodynamicsstellar dynamicsturbulencestars: evolutionstars: interiors
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 98 - 99
Copyright
Copyright © International Astronomical Union 2015 

References

Denissenkov, P. A., Herwig, F., Bildsten, L., & Paxton, B. 2013a, ApJ 762, 8Google Scholar
Denissenkov, P. A., Herwig, F., Truran, J. W., & Paxton, B. 2013b, ApJ 772, 37Google Scholar
Eggenberger, P., Meynet, G., Maeder, A., et al. 2008, Ap&SS 316, 43Google Scholar
Jones, S., Hirschi, R., Nomoto, K., et al. 2013, ApJ 772, 150Google Scholar
Kippenhahn, R., Weigert, A., & Weiss, A. 2013, Stellar Structure and EvolutionGoogle Scholar
Meakin, C. A. & Arnett, D. 2007, ApJ 667, 448Google Scholar