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S. Wende

Research: M-Dwarf Line Formation

Since it is possible to use the narrow and well isolated FeH-Molecule lines in cool stars to determine, for example radial velocities or magnetic field strength and so on, it is necessary to compute these lines from numerical simulations. In my work I will use the line formation program Linfor3D, which is able to compute a spectral line from a three dimensional atmosphere model. This model is computed with the hydrodynamical atmosphere code CO5BOLD. One of the preliminary aims is to investigate, whether it is necessary to use three dimensional models for the line formation or if one dimensional is correct enough. For this purpose I will investigate micro- and macroturbulences in different models with increasing temperature from 2500K to 4000K.

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