Model calculations of magnetic flux tubes. I - Equations and method. II - Stationary results for solar magnetic elements

Details Model calculations of magnetic flux tubes. I - Equations and method. II - Stationary results for solar magnetic elements Model calculations of magnetic flux tubes. I - Equations and method. II - Stationary results for solar magnetic elements

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...139..426d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 139, no. 2, Oct. 1984, p. 426-449. Sponsorship: Deutsche Forschungsgemeinschaf

Statistics

Computation

89

Computational Astrophysics, Magnetic Flux, Magnetohydrodynamics, Photosphere, Solar Atmosphere, Solar Magnetic Field, Baroclinity, Differential Equations, Finite Element Method

Scientific paper

The equations, boundary conditions, geometry, approximations, and numerical methods used in model studies of the physics of magnetic flux tubes in stellar convection zones and atmospheres are presented. The methods described are then used to study the smallest flux tubes in the solar atmosphere, i.e., the magnetic elements that are thought to be responsible for facular points and filigree. The models proposed here are dynamical and include flows; the material properties (e.g., opacity and heat capacity) are calculated self-consistently. Although many limitations remain, it is shown that a considerable contribution to the understanding of the physics of photospheric flux concentrations can be made even at this level of sophistication. In addition, models of stationary magnetic flux elements are presented which are considered to constitute the basic structure of the solar photospheric magnetic field.

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