Other
Scientific paper
Jan 1968
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1968jqsrt...8..317d&link_type=abstract
Journal of Quantitative Spectroscopy and Radiative Transfer, Volume 8, Issue 1, p. 317-322.
Other
6
Scientific paper
During the expansion of a stellar corona (stellar wind), highly charged ions may move faster than protons under the action of thermal diffusion in the temperature gradient region, as well as slower under the action of gravitational separation in the isothermal region. We discuss here the different consequences of these diffusion phenomenas. Noting that the reactions of ionization and recombination have characteristic times which are not small compared to the time for a significant change in the temperature experienced by a single ion, one sees that it is necessary to treat the equations of diffusion together with the equations of ionization. The results are the following:local over abundance of the heavy elements in the corona;stationary state out of local equilibrium, the “apparent temperature” that would be deduced from the ratio of the number density of two successive ions being lower than the electron temperature. Therefore, the interpretation of the eclipse and UV observations of the lower solar corona has to be reconsidered owing to the non-LTE state of a given atom, and to the variation of its abundance with height. The purpose of this paper is to describe some physical phenomena that take place in the transition region between the chromosphere and the corona in the presence of a stellar wind, and the bearing of these on the problem of interpreting coronal emissions.
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