Poster Presentation

From Spectroscopic Abundance Analysis to Radiation-Hydrodynamics of the 0.8 Msun Star

Author(s): Kiehunn Bach (Yonsei University)

Presenter: Kiehunn Bach (Yonsei University)

Based on a well constrained stellar parameters of the binary star (mu Cassiopeiae),
the 3-D Radiation-Hydrodynamic simulations for the surface
convection of the primary star(0.8 Msun) have been computed.
Firstly, chemical abundances of the target stars are determined from the high resolution spectroscopy.
Combining spectro-photometric and astrometric data, physical parameters are calibrated within the framework of standard evolutionary theory.
The best fit model has been utilized as the starting model of the 3-D radiation-hydrodymics for surface convection.
The ultimate goal of this study is to describe physical processes inside stars through a complete modelling.