Volume 504, Number 2, September III 2009
|Page(s)||595 - 603|
|Published online||16 July 2009|
Comparison of the thin flux tube approximation with 3D MHD simulations
Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany e-mail: firstname.lastname@example.org
2 Instituto de Astrofísica de Canarias, C/ Vía Láctea, s/n, 38205 – La Laguna (Tenerife), Spain
3 School of Space Research, Kyung Hee University, Yongin, Gyeonggi 446-701, Korea
Accepted: 3 July 2009
Context. The structure and dynamics of small vertical photospheric magnetic flux concentrations has been often treated in the framework of an approximation based upon a low-order truncation of the Taylor expansions of all quantities in the horizontal direction, together with the assumption of instantaneous total pressure balance at the boundary to the non-magnetic external medium. Formally, such an approximation is justified if the diameter of the structure (a flux tube or a flux sheet) is small compared to all other relevant length scales (scale height, radius of curvature, wavelength, etc.). The advent of realistic 3D radiative MHD simulations opens the possibility of checking the consistency of the approximation with the properties of the flux concentrations that form in the course of a simulation.
Aims. We carry out a comparative analysis between the thin flux tube/sheet models and flux concentrations formed in a 3D radiation-MHD simulation.
Methods. We compare the distribution of the vertical and horizontal components of the magnetic field in a 3D MHD simulation with the field distribution in the case of the thin flux tube/sheet approximation. We also consider the total (gas plus magnetic) pressure in the MHD simulation box.
Results. Flux concentrations with super-equipartition fields are reasonably well reproduced by the second-order thin flux tube/sheet approximation. The differences between approximation and simulation are due to the asymmetry and the dynamics of the simulated structures.
Key words: magnetohydrodynamics (MHD) / Sun: magnetic fields / Sun: photosphere
© ESO, 2009
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