Solar Filament Physiognomy: Inferring Magnetic Quantities from Imaging Observations

Magnetic field is the key physical quantity in solar physics as it controls all kinds of solar activity, ranging from nanoflares to big flares and coronal mass ejections (CMEs). However, so far only the magnetic field on the solar surface can be precisely measured, and the most important coronal magnetic field remains undetectable accurately. Without the knowledge of the coronal magnetic field, it is even more difficult to obtain secondary quantities related to magnetic field, such as the curvature of field lines, magnetic helicity, and magnetic configuration. The prevailing approaches to obtain the coronal magnetic field include coronal magnetic extrapolation. Actually there were continued efforts in coronal seismology to derive the primary quantity, magnetic field, and scattered efforts to derive secondary magnetic quantities based on imaging observations of solar filaments, without the help of polarization measurements. We call this approach solar filament physiognomy. In this paper, we review these efforts made in the past decades, and point out that this approach will be promising as large telescopes are being built and more fine structures of filament channels will be disclosed.