Physics
Scientific paper
Jun 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph...97..283s&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 97, June 1985, p. 283-307. NSF-NASA-DOE-supported research.
Physics
19
Astronomical Models, Magnetohydrodynamic Stability, Solar Prominences, Thermal Stability, Compressibility, Conductive Heat Transfer, Pressure Distribution, Shear Layers, Solar Corona
Scientific paper
Previous studies of a thermal (radiative) instability in a sheared magnetic field have shown that, under solar coronal conditions, cool condensations can form in a small neighborhood about the shear layer. Such results have served to model the formation of solar filaments (or prominences) observed to occur above photospheric magnetic polarity-inversion lines. A surprising conclusion of these studies is that the width of the condensation does not depend on the thermal conductivity (κ∥). By examining the mass-flow patterns of two-dimensional condensations in the absence of thermal conduction, the authors demonstrate that local plasma dynamics and the constraints imposed by boundary conditions are together sufficient to explain the size of the condensation width. The results of a series of numerical calculations which illustrate the characteristic mode structure of sheared-field condensations are presented.
Sparks Lisa
van Hoven Gerard
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