Multi-spacecraft analysis of the solar coronal plasma

This thesis deals with two different approaches in the analysis of the solar corona: an observational and a theoretical one. The first approach aims at the reconstruction of the 3D structure of phenomena in the solar corona using data obtained by multiple spacecraft. The observed and analyzed solar phenomena were prominences and CMEs. For the analysis of the observed phenomena we extended and applied a 3D stereoscopic reconstruction method, called Multi-view B-spline Stereoscopic Reconstruction. The second approach is related to the extrapolation of the coronal magnetic field from a photospheric magnetogram using the a non-linear force-free field model. It is generally accepted that coronal loops observed in EUV images outline magnetic field lines. The results from many conventional magnetic field extrapolations show large discrepancies between the extrapolated magnetic field lines and the observed coronal loops. We therefore introduced an additional observational constraint to the extrapolation scheme by requiring the field also reproduces 3D reconstructed coronal loops. This is achieved by minimizing the local angles between the extrapolated magnetic field and the tangents to the coronal loops. We call this new method stereoscopic – nonlinear force-free field extrapolation method because the shape of the coronal loops is reconstructed by stereoscopy. In the thesis we present the new method and tests of it with synthetic data.