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Hydrodynamic simulations of the core helium flash

Published online by Cambridge University Press:  01 April 2008

Miroslav Mocák
Affiliation:
Max-Planck-Institut für Astrophysik, Postfach 1312, 85741 Garching, Germany email: mmocak@mpa-garching.mpg.de
Ewald Müller
Affiliation:
Max-Planck-Institut für Astrophysik, Postfach 1312, 85741 Garching, Germany email: mmocak@mpa-garching.mpg.de
Achim Weiss
Affiliation:
Max-Planck-Institut für Astrophysik, Postfach 1312, 85741 Garching, Germany email: mmocak@mpa-garching.mpg.de
Konstantinos Kifonidis
Affiliation:
Max-Planck-Institut für Astrophysik, Postfach 1312, 85741 Garching, Germany email: mmocak@mpa-garching.mpg.de
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Abstract

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We desribe and discuss hydrodynamic simulations of the core helium flash using an initial model of a 1.25 M star with a metallicity of 0.02 near at its peak. Past research concerned with the dynamics of the core helium flash is inconclusive. Its results range from a confirmation of the standard picture, where the star remains in hydrostatic equilibrium during the flash (Deupree 1996), to a disruption or a significant mass loss of the star (Edwards 1969; Cole & Deupree 1980). However, the most recent multidimensional hydrodynamic study (Dearborn et al. 2006) suggests a quiescent behavior of the core helium flash and seems to rule out an explosive scenario. Here we present partial results of a new comprehensive study of the core helium flash, which seem to confirm this qualitative behavior and give a better insight into operation of the convection zone powered by helium burning during the flash. The hydrodynamic evolution is followed on a computational grid in spherical coordinates using our new version of the multi-dimensional hydrodynamic code HERAKLES, which is based on a direct Eulerian implementation of the piecewise parabolic method.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2008

References

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