Coronal Holes, Filament Channels And Filaments: Observations Of The Self-organization Of The Coronal Magnetic Field Over Solar Cycles 23 And 24
Abstract
The aim of this work is to understand the relationship between coronal holes, coronal hole boundaries and one of the other main features of the coronal magnetic field, namely filament channels, regions of highly sheared magnetic fields overlying photospheric polarity reversal boundaries. The well-developed filament channel is a necessary ingredient for filament formation. Polar coronal holes and polar crown filament channels always seem to exist together, and even during periods of weakest activity, when nothing indicates the presence of polar crown channels on the solar disk, polar crown prominences appear at the limb proving their existence. Does a similar symbiotic relationship exist also for other coronal holes? There is some indication that for middle and low latitude coronal holes different configurations occur depending on the polarity of the hole relative to the pole. If the polarity is the same, then a coronal pseudostreamer configuration can form with twin filament channels at its base, while if the polarity is opposite, the right conditions for the development of the filament channels and filaments following the hemispheric helicity rule arise. Using SOHO/EIT and MDI, STEREO/EUVI, SDO/AIA and HMI instruments we trace the formation and mutual evolution of coronal holes and their symbiotic filament channels up to and including filament formations, eruptions and subsequent reformations during period 1998-2012 (solar cycles 23 and 24).
- Publication:
-
American Astronomical Society Meeting Abstracts #220
- Pub Date:
- May 2012
- Bibcode:
- 2012AAS...22020202P