Other
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.0203k&link_type=abstract
American Astronomical Society, SPD meeting #37, #2.03; Bulletin of the American Astronomical Society, Vol. 38, p.221
Other
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 in long, low-lying magnetic flux tubes if the heating is localized near the chromosphere. Our previous studies established the effects of steady heating in flux tubes of different geometries. In some 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; in others, static condensations grow as long as the heating continues. Here we will discuss the effects of impulsive heating, as indicated by many coronal-heating models, on the formation and evolution of prominence plasmas.This work was supported by NASA and ONR.
Antiochos Spiro K.
Karpen Judith T.
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