Hydro dynamic simulations of the core helium flash
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 eur new version of the multi-dimensional hydrodynamic code HERAKLES,which is based on a direct Eulerian implementation of the piecewise parabolic method.
Stars:evolution- hydrodynamics-convection
Miroslav Mocák Ewald Müller Achim Weiss Konstantinos Kifonidis
Max-Planck-Institut für Astrophysik,Postfach 1312,85741 Garching,Germany
国际会议
The 252th Symposium of the International Astronomical Union(国际天文学联合会第252届研讨会)
海南三亚
英文
215-222
2008-04-06（万方平台首次上网日期，不代表论文的发表时间）