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Formation of Solar Prominences with Normal and Inverse Polarities

Published online by Cambridge University Press:  12 April 2016

G. S. Choe  and
L. C. Lee
G. S. Choe
Affiliation:
Geophysical Institute, University of Alaska Fairbanks, AK 99775-0800, U.S.A.
L. C. Lee
Affiliation:
Geophysical Institute, University of Alaska Fairbanks, AK 99775-0800, U.S.A.

Abstract

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Numerical simulations of solar prominence formation are presented employing photospheric horizontal motions as boundary conditions. Three different combinations of magnetic field configurations and footpoint motions are considered: (1) a bipolar arcade with a footpoint shear, (2) an arcade exposed to a shearing and converging motion, (3) two adjacent arcades undergoing a shearing and converging motion. In each case, it is found that the dynamic evolution of magnetic fields can force the plasma into a thermal instability leading to the formation of a prominence.

Type
Session 2. Theory of Active Region Structure
Information
International Astronomical Union Colloquium , Volume 141: The Magnetic and Velocity Fields of Solar Active Regions , 1993 , pp. 138 - 142
Copyright
Copyright © Astronomical Society of the Pacific 1993

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