Formation of solar prominences by photospheric shearing motions

Details Formation of solar prominences by photospheric shearing motions Formation of solar prominences by photospheric shearing motions

Apr 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992soph..138..291c&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 138, no. 2, April 1992, p. 291-329. Research supported by NASA.

Physics

57

Magnetohydrodynamics, Photosphere, Solar Corona, Solar Prominences, Solar Temperature, Digital Simulation, Gravitational Fields, Radiant Cooling, Thermal Conductivity

Scientific paper

The formation of the normal polarity solar prominences in a magnetic arcade by photospheric shearing motions was studied using a two-and-a-half-dimensional MHD code, which includes the gravity, radiative cooling, simplified coronal heating, and thermal conduction along the field lines. It was found that a footpoint shear induces an expansion of the magnetic arcade and cooling of the plasma in it; simultaneously, the denser material from the lower part of the arcade is pulled up by the expanding field lines. Thus, a local enhancement of radiative cooling is effected, leading to the onset of thermal instability and the condensation of coronal plasma. The condensed material grows vertically to form a sheetlike structure leading eventually to the formation of prominence.

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