Reconstruction of Solar Coronal Linear Force-Free Magnetic Field

Solar magnetic fields has an important role in the construction of the corona. In the coronal condition, the gas pressure and gravity are neglected as com-paired with the magnetic pressure. Here, the model of Linear Force-Free Field (LFFF) is introduced. Based on this model and appropriate boundary conditions, the structure of coronal magnetic field is reconstructed. First, using semi-analytic Seehafer method, the LFFF is reconstructed using the Wiegelmann code for the line of sight (LOS) magnetogram. Then, the magnetic field lines and loops on a given magnetogram is plotted on the corresponding AIA image for estimating the compatibility. Finally, by calculating the variance between a given traced loop and corresponding reconstructed loops, we find a proper magnetic field parameter for reconstructing a loop before and after flaring.