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Abstract
We present a method to include stereoscopic information about the three dimensional
structure of flux tubes into the reconstruction of the coronal magnetic field. Due
to the low plasma beta in the corona we can assume a force free magnetic field, with
the current density parallel to the magnetic field lines. Here we use linear force
free fields for simplicity. The method uses the line of sight magnetic field on the
photosphere as observational input. The value of \(\alpha\) is determined iteratively
by comparing the reconstructed magnetic field with the observed structures. The final
configuration is the optimal linear force solution constrained by both the photospheric
magnetogram and the observed plasma structures. As an example we apply our method
to SOHO MDI/EIT data of an active region. In the future it is planned to apply the
method to analyse data from the SECCHI instrument aboard the STEREO mission.