Flare loop radiative hydrodynamics. I - Basic methods

Details Flare loop radiative hydrodynamics. I - Basic methods Flare loop radiative hydrodynamics. I - Basic methods

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...265..483m&link_type=abstract

Astrophysical Journal, Part 1, vol 265, Feb. 1, 1983, p. 483-506.

Mathematics

40

Chromosphere, Coronal Loops, Magnetohydrodynamic Stability, Radiative Transfer, Solar Flares, Thermal Stability, Conductive Heat Transfer, Eigenvalues, Energy Transfer, Finite Difference Theory, Magnetohydrodynamic Flow, Matrices (Mathematics), Solar Atmosphere, Solar Physics, Solar Spectra, Space Plasmas, Stellar Models

Scientific paper

The study presented here has two goals. The first is to examine the role of energy transport mechanisms in flare dynamics, for instance, thermal cone conduction in the corona and radiative transfer in the chromosphere. The second is to provide diagnostics of flare energization processes by predicting the evolutionary behavior of concurrent emissions from all regions of the flaring atmosphere. To attain these ends, a numerical method is developed for the simultaneous solution of thy continuity, momentum, and energy equations; the time-dependent atomic rate equations describing ionization and excitation; and the radiative transfer equations. With the physical model and computational methods used here, all components of the plasma move as a single fluid and in the initial studies are assumed to have a common kinetic temperature. The plasma is constrained to move in one dimension along the axis of a loop of nonuniform cross section, the geometry of which is defined by a sufficiently strong magnetic field.

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