Solar transition region response to variations in the heating rate

Details Solar transition region response to variations in the heating rate Solar transition region response to variations in the heating rate

Apr 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...255..783m&link_type=abstract

Astrophysical Journal, Part 1, vol. 255, Apr. 15, 1982, p. 783-796. Navy-NASA-sponsored research.

Astronomy and Astrophysics

Astrophysics

60

Chromosphere, Solar Corona, Solar Temperature, Stellar Models, Atmospheric Temperature, Coronal Loops, Hydrodynamic Equations, Ion Production Rates, Magnetic Flux, Magnetohydrodynamics, Nonequilibrium Plasmas, Periodic Variations, Temperature Distribution, Temperature Gradients, Time Dependence

Scientific paper

The response of a numerical model for the upper chromosphere, transition region, and corona to variations in the energy input has been examined. The numerical model solves the set of one-dimensional two-fluid hydrodynamic equations in a simple vertical magnetic flux tube. The atmosphere responds to both the increase and decrease in energy deposition by smoothly readjusting the temperature gradient and the amount of material in the region of peak radiating efficiency to radiate away energy being deposited. At no time during this readjustment is a departure from a thin laminar transition region structure seen. In addition, a time-dependent description of the nonequilibrium ionization of all of the ionization stages of oxygen has been included. This calculation is coupled with the self-consistent calculations of the dynamical variables. It is found that the nonequilibrium ionization balance calculations for both heating and cooling small loops in the quiet sun predict relative ionic abundances which differ substantially from those which would be predicted by an equilibrium calculation

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