The growth of radiative filamentation modes in sheared magnetic fields

Details The growth of radiative filamentation modes in sheared magnetic fields The growth of radiative filamentation modes in sheared magnetic fields

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986nascp2442...27v&link_type=abstract

In NASA. Goddard Space Flight Center Coronal and Prominence Plasmas p 27-31 (SEE N87-20871 13-92)

Physics

Conductive Heat Transfer, Plasmas (Physics), Solar Corona, Solar Magnetic Field, Solar Physics, Solar Prominences, Rates (Per Time), Thermal Stability, Thermodynamics

Scientific paper

Observations of prominences show them to require well-developed magnetic shear and to have complex small-scale structure. Researchers show here that these features are reflected in the results of the theory of radiative condensation. Researchers studied, in particular, the influence of the nominally negligible contributions of perpendicular (to B) thermal conduction. They find a large number of unstable modes, with closely spaced growth rates. Their scale widths across B show a wide range of longitudinal and transverse sizes, ranging from much larger than to much smaller than the magnetic shear scale, the latter characterization applying particularly in the direction of shear variation.

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