Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005apj...634.1395w&link_type=abstract
The Astrophysical Journal, Volume 634, Issue 2, pp. 1395-1404.
Astronomy and Astrophysics
Astronomy
25
Magnetohydrodynamics: Mhd, Sun: Activity, Sun: Magnetic Fields, Sun: Prominences
Scientific paper
To investigate the hypothesis that prominences form by magnetic reconnection between initially distinct flux systems in the solar corona, we simulate coronal magnetic field evolution when two flux systems are driven together by boundary motions. In particular, we focus on configurations similar to those in the quiescent prominence formation model of Martens & Zwaan. We find that reconnection proceeds very weakly, if at all, in configurations driven with global shear flows (i.e., differential rotation); reconnection proceeds much more efficiently in similar configurations that are driven to collide directly, with converging motions along the neutral line that lead to flux cancellation; reconnected fields from this process can exhibit sheared, dipped field lines along the neutral line, consistent with prominence observations. Our field configurations do not possess the ``breakout'' topology, and eruptions are not observed, even though a substantial amount of flux is canceled in some runs.
Antiochos Spiro K.
DeVore Richard C.
Welsch Brian Thomas
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