Physics
Scientific paper
May 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsp21b..02k&link_type=abstract
American Geophysical Union, Spring Meeting 2005, abstract #SP21B-02
Physics
7507 Chromosphere, 7509 Corona, 7531 Prominence Eruptions
Scientific paper
Prominences are among the most spectacular manifestations of both quiescent and eruptive solar activity, yet the origins of their magnetic-field and plasma structures remain poorly understood. We have made steady progress toward a comprehensive model of prominence formation and evolution with our sheared 3D arcade model for the magnetic field and our thermal nonequilibrium model for the cool, dense material suspended in the corona. According to the thermal nonequilibrium model, condensations form readily along long, low-lying magnetic field lines if the heating is localized near the chromosphere. In most cases this process yields a dynamic cycle in which condensations repetitively form, stream along the field line, and ultimately disappear by falling onto the nearest footpoint. Two key observed features were not adequately explained by our earlier simulations of thermal nonequilibrium, however: the thread-like (i.e., elongated) horizontal structure and high-speed motions of many condensations. Here we discuss how simple modifications to our model largely eliminate these discrepancies, strengthening the case for thermal nonequilibrium as the origin of prominence condensations and for low-twist models of prominence magnetic structure. This work was supported by NASA and ONR.
Antiochos Spiro
Karpen Judith
Klimchuk James
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