Flare loop radiative hydrodynamics. IV - Dynamic evolution of unstable semiempirical loop models

Details Flare loop radiative hydrodynamics. IV - Dynamic evolution of unstable semiempirical loop models Flare loop radiative hydrodynamics. IV - Dynamic evolution of unstable semiempirical loop models

Apr 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...267..421a&link_type=abstract

Astrophysical Journal, Part 1, vol. 267, Apr. 1, 1983, p. 421-432.

Astronomy and Astrophysics

Astrophysics

19

Chromosphere, Coronal Loops, Hydrodynamic Equations, Magnetohydrodynamic Stability, Radiative Transfer, Solar Flares, Atmospheric Models, Evolution (Development), Nonlinear Equations, Semiempirical Equations, Solar Corona

Scientific paper

The evolution of the unstable solar atmosphere into the nonlinear phase, in response to various perturbations, is followed. The initial dynamic evolution of the atmosphere follows the predictions of linear stability analysis. In the nonlinear phase, rapid changes are confined to the transition region; these changes are manifested as a propagation of the transition region through the plasma, i.e., chromospheric evaporation or condensation. Global evolution therefore proceeds on the coronal conductive time scale. The rate of propagation of the transition region is determined by the imbalance between the energy supplied by thermal conduction from the corona and radiative cooling within the transition region itself. Flow velocities in the lower corona during evaporation or condensation are, in the cases studied, of order 3 km/s. The observed dynamic evolution is consistent with the existence of relatively long-lived coronal loops whose brightnesses vary on the evaporative time scale.

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