Including stereoscopic information in the reconstruction of coronal magnetic fields

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.

18 pages, 7 figures

Cited by in corpus (25)

• Optimization code with weighting function for the reconstruction of coronal magnetic fields
• Nonlinear force-free modeling of the solar coronal magnetic field
• Solar Force-free Magnetic Fields
• Comparing magnetic field extrapolations with measurements of magnetic loops
• An optimization principle for the computation of MHD equilibria in the solar corona
• Magnetic Field Extrapolations in the Corona: Success and Future Improvements
• Guiding Nonlinear Force-Free Modeling Using Coronal Observations: First Results Using a Quasi Grad-Rubin Scheme
• Magnetic modelling and tomography: First steps towards a consistent reconstruction of the solar corona
• On the extrapolation of magneto-hydro-static equilibria on the sun
• Upflows in funnel-like legs of coronal magnetic loops
• First 3D Reconstructions of Coronal Loops with the STEREO A+B Spacecraft: IV. Magnetic Modeling with Twisted Force-Free Fields
• A Nonlinear Force-Free Magnetic Field Approximation Suitable for Fast Forward-Fitting to Coronal Loops. I. Theory
• How to use magnetic field information for coronal loop identification?
• Magneto-static modelling from SUNRISE/IMaX: Application to an active region observed with SUNRISE II
• Magnetic Stereoscopy
• Comparison of Two Coronal Magnetic Field Models for Reconstructing a Sigmoidal Solar Active Region With Coronal Loops
• A Nonlinear Force-Free Magnetic Field Approximation Suitable for Fast Forward-Fitting to Coronal Loops. II. Numeric Code and Tests
• Emission heights of coronal bright points on Fe XII radiance map
• Nonlinear force-free coronal magnetic stereoscopy
• New views on the emission and structure of the solar transition region
• Formation Heights of Extreme Ultraviolet Lines in an Active Region Derived by Correlation of Doppler Velocity and Magnetic Field
• Radiance and Doppler shift distributions across the network of the quiet Sun
• Study of the three-dimensional shape and dynamics of coronal loops observed by Hinode/EIS
• Stereoscopic Measurements of Coronal Doppler Velocities
• The chromospheric component of coronal bright points. Coronal and chromospheric responses to magnetic-flux emergence