Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...280..391v&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 280, May 1, 1984, p. 391-398. NASA-NSF-supported research.
Astronomy and Astrophysics
Astrophysics
15
Magnetohydrodynamic Stability, Solar Corona, Solar Flares, Solar Magnetic Field, Solar Prominences, Tearing Modes (Plasmas), Coupled Modes, Plasma Equilibrium, Plasma Radiation, Radiative Heat Transfer, Resistance Heating
Scientific paper
The way in which the initial development of solar filament radiative cooling and the magnetic reconnection of a solar flare can occur in the center of a field-shear layer is demonstrated. Since the present treatment unites these two mechanisms, it indicates the common as well as the disparate features they possess. Unstable radiation serves to increase the Coulomb resistivity at the X-point, so that the reconnection is not self-quenching. The surprising dominance of the magnetic component of the perturbation in the midwavelength range indicates the need to examine the nonlinear saturation of the energy transport of the radiative mode, taking the accompanying magnetic reconnection and potential-energy release into account, for comparison with observations of filaments as well as for clues to the character of the preflare state.
Steinolfson Richard S.
Tachi Tomohiro
van Hoven Gerard
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