EXTRAPOLATION OF THE SOLAR CORONAL MAGNETIC FIELD FROMSDO/HMI MAGNETOGRAM BY A CESE-MHD-NLFFF CODE

Reconstruction of Solar Coronal Linear Force-Free Magnetic Field

reconstruction of solar coronal linear force-free magnetic field

Potential Field Extrapolation Using Three Components of Solar Vector Magnetogram with a Finite Field of View G. Allen Gary

Abstract. The potential magnetic field from a finite planar boundary is extrapolated into the upper hemisphere using all three of the magnetic field components. The method determines, first, the transverse field assoicated with the observed normal magnetic intensity, and, then by subtraction, the method determines the associated transverse magnetic field observed in the interior (i.e., in the f...

An MHD model for solar coronal plumes

Solar coronal plumes are modelled by solving the steady, ideal, 2-D, magnetohydrodynamic (MHD) equations and assuming azimuthal symmetry around the plume axis. Since magnetic fields are believed to play an essential role in plume formation and structure, a self-consistent method of linearisation of the MHD equations with respect to the magnetic field has been considered here. This consists of t...

The Solar Coronal Magnetic Field Measurements With SOLARC

Direct solar coronal magnetic field measurements have become possible since recent development of high-sensitivity infrared detection technology. The SOLARC instrument installed on Mt. Haleakala is such a polarimetric coronagraph that was designed for routinely observing Stokes parameter profiles in near infrared (NIR) wavelengthes. The Fe 1075 nm forbidden coronal emission line (CEL) is potent...