CHARGE-EXCHANGE NEAR MARS - THE SOLAR-WIND ABSORPTION AND ENERGETIC NEUTRAL ATOM PRODUCTION

Charge exchange between solar wind protons and neutral atmospheric ato ms is expected to affect the solar wind interaction with Mars, but its influences and significance have only been touched upon in previous w ork. Here several features associated with the charge exchange process between the solar wind protons and Martian neutral upper atmospheres are described. The analysis is based on an empirical proton model deri ved from Phobos 2 observations interacting with the Martian atomic (H) and molecular (H-2) hydrogen, and oxygen (O) upper atmospheres repres enting solar minimum and solar maximum conditions. The region where th e largest fraction of solar wind protons is lost by the charge exchang e process is found to be a thin layer above the surface of Mars on the dayside resulting from charge exchange with the thermal oxygen. In ge neral, the magnetosheath and ''magnetosphere'' (where the observed pla sma takes on a different character in the Phobos 2 data) produce two d istinguishable regions where the loss rate of solar wind protons is hi ghest. Increasing solar activity increases the loss rate in the magnet osheath but decreases it in the magnetosphere. No significant increase of the absorption of the solar wind was found near the ''magnetopause '' suggesting that the decrease of the solar wind protons observed by Phobos 2 are not due to the charge exchange process. In addition to a reduction in the solar wind density, the charge exchange reaction resu lts in energetic neutral atom (ENA) production. This paper considers s ome of the detailed properties expected for the ENA population at Mars . The ENA differential fluxes were found to be typically 10(6)-10(7) c m(-2) s(-1) keV(-1) in the energy range 0.01 - 1 keV. During solar min imum, the ENA production rate and ENA integral fluxes were found to be highest in the magnetosheath. At solar maximum the ENA production rat e is highest in the magnetosphere, and ENA integral fluxes in the days ide magnetosphere appear to become comparable to the fluxes in the mag netosheath if the proton temperature in the magnetosphere is low. It i s found that 1-3% of the original solar wind proton flux converts into ENAs before the bow shock. The ENAs produced upstream are undeflected and so may precipitate into the Martian upper atmosphere, depositing an energy flux of up to 3x10(9) eV cm(-2) s(-1) derived from the solar wind. These results both suggest the possible benefits of observing E NA fluxes around Mars and suggest the necessary parameters for detecto r design.