Solar Coronal Modelling Based on Observed Photospheric Magnetic Fields Including the Microphysics of Reconnection

JOERG BUECHNER

Photosphere, chromosphere and corona are coupled by the solar magnetic field. Since direct measurements of chromospheric and coronal magnetic fields usually are not available most investigations of the solar atmospheric magnetic field mathematically extrapolate the photospheric magnetic field to chromosphere and corona. In order to solve the mathematical problem the assumption of force-free fields is used. This excludes Lorentz-forces, i.e. the extrapolation approach neglects a major physical mechanisms of, e.g., coronal heating or solar wind acceleration. Contrary, realistic models have to take into account the plasma pressure and dynamics as well as perpendicular currents (Lorentz-forces!).

We review current achievements in the approach to a physical solar magnetic field modelling and to solar magnetic reconnection by numerical simulation which couples MHD to plasma microphysics, based on solar magnetic field observations. For the introduction of we investigate comparatively LCT, ILCT and MEF methods to derive the photospheric plasma motion.

Solar-B with its opportunities for vector magnetic field measurements and rich onboard plasma diagnostics will provide excellent opportunities to fully utilze the new achievement of solar magnetic field and plasma modelling

Correspondence

BUECHNER JOERG (buechner@linmpi.mpg.de), MAX-PLANCK-INSTITUT FUER SONNENSYSTEMFORSCHUNG

presentation

invited