Effects of diffusion and mass flows on C IV and SI IV lines formed in the solar atmosphere

Details Effects of diffusion and mass flows on C IV and SI IV lines formed in the solar atmosphere Effects of diffusion and mass flows on C IV and SI IV lines formed in the solar atmosphere

Nov 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...250..408r&link_type=abstract

Astrophysical Journal, Part 1, vol. 250, Nov. 1, 1981, p. 408-422.

Astronomy and Astrophysics

Astrophysics

10

Atmospheric Models, Ionic Diffusion, Mass Flow, Solar Atmosphere, Solar Spectra, Ultraviolet Spectra, Abundance, Carbon Isotopes, Line Spectra, Silicon Isotopes, Tables (Data)

Scientific paper

A model for the transition region is derived from an initial interpretation of EUV observations, assuming ionization equilibrium and constant elemental abundance with height. The effects of diffusion and mass flows are then included in the initial model and the emergent profiles of several C IV and Si IV lines are computed. It is found that diffusion and mass flows have a strong effect on both the emergent intensity and spectral shape of these lines. Diffusion acts to deplete the transition region of heavy ions to an extent which depends on the detailed temperature and density structure. The net effect is a weighting of the coronal emission relative to that in the transition. On the basis of the results, it is suggested that the downflows observed in the network in lines of C IV and Si IV could be due to gravitational settling of the ions following their injection, via diffusion, into the corona from spicules. When flows are superposed on the basic diffusion model, the rapid change in elemental abundance characteristic of the model is virtually eliminated and the coronal contribution to the emission in C IV and Si IV lines becomes negligible relative to that in the transition region. Flows have a strong effect on the computed line intensities and introduce large asymmetries into the line shapes.

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