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A. Seelmann

Research: Velocity fields in 3D radiative transport

I am working on the stellar atmosphere code PHOENIX, which is a computer code to model stellar atmosphere. The new part of the code allows to compute 3D models with scattering in the continuum and line in different geometries: Spherical, Caertesian, Cartesian with Periodic Boundary Conditions and Cylindrical. My tasks is from theorical nature: I am working on including the physical treatment of arbitrary velocity fields (Wind) in the observers frame in the code. This is a first step towards realistic 3D hydrodynamical models (from e.g. the Sun) which naturally have a intrinsic velocity field. The new method can also be used to figure out the influence of a moving interstellar medium upon the radiation field from a star or extrasolar planet behind it.