An investigation and analysis of the density and thermal balance of the Martian ionosphere

Details An investigation and analysis of the density and thermal balance of the Martian ionosphere An investigation and analysis of the density and thermal balance of the Martian ionosphere

Jul 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979stin...7931123r&link_type=abstract

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Atmospheric Density, Ion Density (Concentration), Ion Temperature, Mars Atmosphere, Planetary Ionospheres, Thermosphere, Aeronomy, Electron Energy, Energetic Particles, Exothermic Reactions, Reaction Kinetics, Solar Wind

Scientific paper

The major photochemistry consisted of solar EUV and photoelectrons comprising 70 percent and 30 percent respectively, of the initial source of CO2(+) and O(+). The energetic O2(+) provided a substantial source of energy to the ambient ions, distributing of the order of 1.6 x 10 to the -7 power W/sq m at an average of 160 km. This input can be compared to that from the ambient electrons of 1.3 x 10 to the -7 power W/sq m with average deposition at 145 km and from the calculated thermal conduction of 1 x 10 to the -9 power W/sq m at 270 km and 1 x 10 to the -8 power at 230 km for assumed dip angles of 2 deg and 12 deg respectively, for a 10nT magnetic field. At altitudes above 250 km upward, vertical fluxes of the order 6 x 10 to the 10th power/sq m/sec for the thermal ions were calculated. The net ionization of O(+) and CO2(+) by charge exchange with incoming solar wind protons varied from 5 x 10 to the 8th power to 5 x 10 to the 12th power /sq m/sec for assumed field strengths of 50nT to 2nT on the dayside of the planet.

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