アイテム詳細

要旨

For understanding the physical processes in the solar corona, it is helpful to reconstruct the 3D-distribution of plasma density and temperature. We introduce a new iterative method that uses multi-filter observations and an extrapolated coronal magnetic field to fit the physical parameters along the field lines to the observations. Since a model is applied only for the field extrapolation but not to the loops themselves, non-stationary plasma configurations along the loops can be captured. We demonstrate the performance of our code on a self-made model active-region corona and on active region (AR) 11087 observed by the Solar Dynamics Observatory and the Solar Terrestrial Relation Observatory-A in 2010. In the coronal parts of the model AR, the 25% quantile of the deviations of the reconstructed densities relative to the model values is −0.5 to −0.6 below the model values, the 75% quantile being 0.3. Likewise, for the logarithm of the temperature, the same quantiles are at minus and plus 0.04, respectively, relative to the model values. For AR 11087, the seven channels of the Atmospheric Imaging Assembly in the extreme ultraviolet are reproduced very well. For the four channels of the Extreme Ultra Violet Imager in that regime, the synthesised images are slightly brighter than the observations. The structure of the AR can still be identified here.