Computer simulations of the gas flows present todays physically most advanced models of stellar surface convection (granulation). Despite their enormous predictive power they have not yet become a standard ingredient in the broader astrophysical field of stellar structure modeling. This is due to the high computational demands that are involved in their construction. Motivated to promote the inclusion of results from flow simulations, it is intended to investigate in how far less demanding radiation-hydrodynamics (RHD) models restricted to two spatial dimensions (2D) can be utilized to get quantative estimates of relevant stellar properties. This will be tested by a differential comparison between 2D and 3D RHD models. It is planned to study a small, carefully selected sample of objects in the Hertzsprung-Russell diagram which give particularly clear evidence for the issue in the covered parameter space. The results will enable us to assess the quality of already existing 2D results, and may make the production of RHD model grids much faster. The applicant expects in first place the broadening of his knowledge in numerical methods and programming techniques. The NBIfAFG group has ample experience in the handling of massively parallel machines. These will play an important role in the development of numerical RHD in the future. From the physical point of view the proposed project complements nicely the ongoing activities of the applicant's current research group. The visit will certainly strengthen the ties between the two groups and thus leads to a more economical utilization of human resources.
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