Astronomy and Astrophysics – Astronomy
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.5807m&link_type=abstract
American Astronomical Society Meeting 210, #58.07; Bulletin of the American Astronomical Society, Vol. 39, p.168
Astronomy and Astrophysics
Astronomy
Scientific paper
Coronal mass ejections (CMEs) have the property that they originate from over photospheric magnetic polarity inversion lines (PILs) where the magnetic field is nearly horizontal and parallel to the PIL. Shear flows are often observed to occur along the PIL prior to and during CMEs, and such flows have been artificially applied for decades to model flares and CMEs. This talk will build on the recent discovery that such shearing motions are driven by the the Lorentz force that naturally arises when bipolar magnetic fields emerge into the corona. Here we will show that shearing motions cause a magnetic flux rope to partially erupt allowing the upper extremity of the rope to fully separated from the portion still bound to the photosphere. The eruption occurs as shearing motions transport axial flux and energy from the submerged portion of the field to the expanding portion, strongly coupling the solar interior to the corona. The eruption mechanism readily explains the initiation of CMEs as well as many observations associated with CMEs most notably shear flows and the concentration of magnetic shear near the PIL where prominences form. The separation of the rope leaving flux attached to the photosphere naturally explains the partial eruption of filaments and how filament channels remain intact to spawn multiple CMEs.
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