Using Coronal Cells to Infer the Magnetic Field Structure and Chirality of Filament Channels

Abstract

Coronal cells are visible at temperatures of ~ 1.2 MK in Fe XII coronal images obtained from the Solar Dynamics Observatory (SDO) and Solar Terrestrial Relations Observatory (STEREO) spacecraft. We show that near a filament channel, the plumelike tails of these cells bend horizontally in opposite directions on the two sides of the channel like fibrils in the chromosphere. Because the cells are rooted in magnetic flux concentrations of majority polarity, these observations can be used with photospheric magnetograms to infer the direction of the horizontal field in filament channels and the chirality of the associated magnetic field. This method is similar to the procedure for inferring the direction of the magnetic field and the chirality of the fibril pattern in filament channels from H-alpha observations. However, the coronal cell observations are easier to use and provide clear inferences of the horizontal field direction for heights up to ~ 50 Mm into the corona.

accepted for publication in The Astrophysical Journal

References in corpus (3)

• Observations and Magnetic Field Modeling of a Solar Polar Crown Prominence
• Origins of Rolling, Twisting and Non-Radial Propagation of Eruptive Solar Events
• Evidence for polar jets as precursors of polar plume formation

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