Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...333.1069p&link_type=abstract
Astronomy and Astrophysics, v.333, p.1069-1081 (1998)
Astronomy and Astrophysics
Astrophysics
9
Sun: Chromosphere, Sun: Abundances, Solar Wind
Scientific paper
A multi-fluid model for a hydrogen-helium mixture in an ionization-diffusion layer in the (solar) chromosphere is presented. The purpose of this model is to serve as a background for fractionation models calculating the abundance variations of minor species from the photosphere to the solar wind. The emphasis will be on the determination of the (mean) flow velocity in that ionization layer. The equations of continuity and momentum of every component, neutral and (singly) ionized for both elements, will be solved together with an energy equation including heating and radiative losses. Special attention will be paid to the ionization and the elastic collisions as well as to resonant charge exchange. One of the main results is the connection of the particle flux through the chromosphere with the ionization rate, i. with the photon flux in the UV. Furthermore the abundance variations of helium are discussed with the result, that the ion-neutral separation processes leading to the fractionation of the minor elements cannot explain the fractionation of helium as measured in the solar wind.
Marsch Eckart
Peter Hardi
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