||Kühner, O. 1, Utz, D. 1,2,3, Muller, R. 4, Van Doorsselaere T. 3, Magyar, N. 3, Veronig, A. 1, Campos Rozo, J. I. 1,5, Jelinek, P. 6, Krikova, K. 1 Affiliations: 1) IGAM/Institute of Physics, Karl-Franzens University Graz, Austria 2) Instituto de Astrofísica de Andalucía IAA/CSIC, Granada, Spain 3) Centre for mathematical Plasma Astrophysics CmPA, KU-Leuven, Leuven, Belgium 4) Observatoire Pic du Midi, University of Toulouse, France 5) Observatorio Astronomico Nacional - Universidad Nacional de Colombia 6) Institute of Physics, University of South Bohemia, Czech Republic
||The solar atmosphere is structured by magnetic fields often resembling in the lower atmosphere vertical flux tubes opening with height. While these flux tubes are observed with photospheric cross-section magnetic field strengths going well beyond the kG range, in most models field strengths of only a few hundred Gauss are used. This has to do with the problems (stratified densities, pressures and energies) arising in constructing strong vertical opening flux tubes while keeping magneto-static conditions for the whole atmosphere.
Reaching higher field strengths while keeping magneto-static conditions in models is of utmost importance as simulations of wave transport but also the formation of spectral lines is dependent on the stratification of the atmosphere and the flux tube parameters.
We will introduce here our novel approach for modelling more realistic magnetic flux tubes (with magnetic field strengths beyond the kG range).
By varying input parameters for this model (like field strength, horizontal radius, opening with height, internal stratification) we are able to investigate the formation heights of spectral lines as well as to simulate wave transport mechanisms within magnetic flux tubes with different shapes and field strengths.
We will outline our approach and show first results for the formation heights of spectral lines as a function of the varying input parameters.