THE MAGNETIC STRUCTURE OF SOLAR PROMINENCE CAVITIES: NEW OBSERVATIONAL SIGNATURE REVEALED BY CORONAL MAGNETOMETRY

Reconstruction of Solar Coronal Linear Force-Free Magnetic Field

Observations of Solar Coronal Magnetic

This review discusses methods for determining solar coro-nal magnetic elds, with an emphasis on radio measurements of eld strengths in solar active regions.

Prominence and Filament Magnetometry Simulations

The simulations reported in this Note cover the cases of both prominence (i.e., off-limb) and filament (i.e., on-disk) observations. The various plots illustrate the statistics of the inversion of the magnetic topology—field strength (B), LOS inclination (ΘB), and POS direction (ΦB)— from different sets of 2700 synthetic observations, in the form of error scatter plots (top panels) and error hi...

Editorial: Coronal Magnetometry

Coronal transverse magnetohydrodynamic waves in a solar prominence.

Solar prominences are cool 10(4) kelvin plasma clouds supported in the surrounding 10(6) kelvin coronal plasma by as-yet-undetermined mechanisms. Observations from Hinode show fine-scale threadlike structures oscillating in the plane of the sky with periods of several minutes. We suggest that these represent Alfvén waves propagating on coronal magnetic field lines and that these may play a role...