Simulations of magnetoconvection in cool main-sequence stars
2014
In this thesis, the magnetoconvective processes in the nearsurface
layers of cool main-sequence stars were studied in 24
three-dimensional local “box-in-a-star” simulations. For each of
six sets of stellar parameters corresponding to spectral types
F3V –M2V including the solar case (G2V), one non-magnetic and
three magnetic simulations with an initially vertical and homogeneous
field of 20, 100, and 500G were performed.
A granule segmentation and tracking algorithm was developed
and the granulation was analysed for the non-magnetic and some
magnetic runs. For a few wavelength passbands, the centre-tolimb
variation of the intensity and its rms contrast were calculated
on the basis of snapshots from the simulations. Synthetic spectral
line profiles were calculated for the simulated stars. A discintegration
including differential rotation was carried out in order
to study the effects of the three-dimensional atmospheric structure
on spectral line profiles.
The simulations presented in this thesis are an essential step
towards a physically comprehensive description of magnetoconvective
processes in stars, which is needed, e. g. for the improvement
of inversion methods and the correct interpretation of spectroscopic
observations.
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