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Hydrodynamic Processes in Massive Stars

Published online by Cambridge University Press:  01 April 2008

Casey A. Meakin
Casey A. Meakin*
Affiliation:
Astronomy Department, University of Arizona, Tucson, AZ 85721, USA Astronomy and Astrophysics Center, University of Chicago, Chicago, IL 60637, USA Joint Institute for Nuclear Astrophysics, University of Chicago, Chicago, IL, 60637, USA email: casey.meakin@gmail.com
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Abstract

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The hydrodynamic processes operating within stellar interiors are far richer than represented by the best stellar evolution model available. Although it is now widely understood, through astrophysical simulation and relevant terrestrial experiment, that many of the basic assumptions which underlie our treatments of stellar evolution are flawed, we lack a suitable, comprehensive replacement. This is due to a deficiency in our fundamental understanding of the transport and mixing properties of a turbulent, reactive, magnetized plasma; a deficiency in knowledge which stems from the richness and variety of solutions which characterize the inherently non-linear set of governing equations. The exponential increase in availability of computing resources, however, is ushering in a new era of understanding complex hydrodynamic flows; and although this field is still in its formative stages, the sophistication already achieved is leading to a dramatic paradigm shift in how we model astrophysical fluid dynamics. We highlight here some recent results from a series of multi-dimensional stellar interior calculations which are part of a program designed to improve our one-dimensional treatment of massive star evolution and stellar evolution in general.

Keywords

Hydrodynamicsconvectionstars: evolutionmethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 439 - 449
Copyright
Copyright © International Astronomical Union 2008

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