Diffusion effects on the helium abundance of the solar transition region and corona

Details Diffusion effects on the helium abundance of the solar transition region and corona Diffusion effects on the helium abundance of the solar transition region and corona

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...402..334h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 402, no. 1, p. 334-343.

Statistics

Computation

17

Conservation Equations, Gaseous Diffusion, Helium, Plasma Dynamics, Solar Corona, Abundance, Computational Grids, Hydrogen Plasma

Scientific paper

The diffusion of helium in the solar transition region is studied by solving the mass and momentum conservation equations for a hydrogen-helium plasma given a representative temperature profile. Steady state solutions show that two distinct atmospheres may result. In cases where the thermal force on alpha-particles is balanced by the partial pressure gradient force, helium is the dominant coronal species. On the other hand, if it is the frictional force between protons and alpha-particles which balances the thermal force on alpha-particles then hydrogen is the major coronal component. In order to explore which of these solutions are attainable within reasonable time scales, the time-dependent equations are solved, starting from an initial state with a uniform helium abundance of 10 percent. The atmosphere as a whole is close to hydrostatic equilibrium, but due the thermal forces the individual elements are not. This force inbalance leads to a differential flow between species. It is found that this differential flow leads to a significant enhancement of the coronal helium abundance. Even for the relatively shallow temperature gradient used the helium abundance in the lower corona increases to 30 percent over a 24 hr period.

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