Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...236..270a&link_type=abstract
Astrophysical Journal, Part 1, vol. 236, Feb. 15, 1980, p. 270-279.
Astronomy and Astrophysics
Astrophysics
13
Cold Plasmas, Magnetohydrodynamic Flow, Solar Prominences, Stellar Models, Cooling, H Alpha Line, Magnetohydrodynamic Stability, Solar Flares, Velocity Distribution
Scientific paper
A one-dimensional numerical model of active loop prominences is investigated. The model includes the effects of gravity, the geometry of the magnetic field, and conduction losses to the chromosphere. Calculations indicate that, as originally proposed by Goldsmith, the thermal instability mechanism is, by itself, sufficient to account for the appearance of bright H-alpha knots in postflare loops. Under certain conditions, initial perturbations in the loop temperature and density profiles of small, but finite, amplitude (approximately 5%) and large size scale (greater than or approximately equal to 10 to the 9th cm) can grow into condensations with temperature and density differences of over an order of magnitude and size scales of less than 10 to the 8th cm. In agreement with observations, the conditions that must be satisfied are such that loop prominence systems are likely to occur only in large flares and such that knots preferentially form at the tops of loops. The velocities, densities, and lifetimes calculated for the loop material are also in agreement with observations. It is concluded that in order for H-alpha knots to occur, heating of some form must continue into the late cooling phase of a flare loop, and that this heating is more intense near the loop base than near the apex.
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