Closed coronal structures. V - Gasdynamic models of flaring loops and comparison with SMM observations

Details Closed coronal structures. V - Gasdynamic models of flaring loops and comparison with SMM observations Closed coronal structures. V - Gasdynamic models of flaring loops and comparison with SMM observations

Jul 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...270..270p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 270, July 1, 1983, p. 270-287. Research supported by the Consiglio Nazional

Astronomy and Astrophysics

Astrophysics

81

Chromosphere, Magnetohydrodynamics, Solar Corona, Solar Maximum Mission, Solar X-Rays, Atmospheric Density, Atmospheric Models, Atmospheric Temperature, Light Curve, Line Spectra, Solar Flares

Scientific paper

The hydrodynamic response of confined magnetic structures to strong heating perturbations is investigated by means of a time-dependent one-dimensional colde which incorporates the energy, momentum, and mass conservation equations. The entire atmospheric structure from the chromosphere to the corona is taken into account. Models with different energy input, heating time dependence, preflare conditions and heating location have been examined in the numerical simulations.
The result of model calculations are compared with observations of flares obtained with the X-ray Polychromator experiment on the Solar Maximum Mission. These include light curves of spectral lines formed over a wide range of coronal flare temperatures, as well as determinations of Doppler shifts for the high temperature plasma. Several examples are used to illustrate the range of the observational variation.
It is shown that the predictions of the numerical simulations are in good overall agreement with the observed evolution of the flare coronal plasma. The model reproduces correctly the temporal profile of X-ray spectral lines and -- to first order at least -- their relative intensities. The upflow velocities predicted by model calculations are in agreement with the observed blueshifts, supporting the interpretation of the blueshifts as due to evaporation of chromospheric material. The possibility of using the comparison of model predictions with observations to derive information on the processes of energy release and transfer in solar flares is discussed.

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