Physics
Scientific paper
Feb 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991jgr....96.1819l&link_type=abstract
Journal of Geophysical Research (ISSN 0148-0227), vol. 96, Feb. 1, 1991, p. 1819-1825.
Physics
66
Energy Spectra, Mars Atmosphere, Planetary Atmospheres, Recombination Reactions, Titan, Monte Carlo Method, Nitrogen, Oxygen, Planetary Magnetospheres, Solar Wind, Planets, Satellites, Mars, Titan, Atmosphere, Saturn, Escape, Flux, Energy, Spectra, Particles, Concentration, Oxygen, Nitrogen, Coronas, Ions, Calculations, Monte Carlo Method, Comparisons, Electrons, Mass, Impact Effects, Ionization, Solar Wind, Magnetosphere, Mass Loading, Altitude, Density, Distribution, Diagrams, Interaction, Chemical Reacti
Scientific paper
Energy flux spectra and particle concentrations of the hot O and N coronae from Mars and Titan, respectively, resulting primarily from dissociative recombination of molecular ions, have been calculated by means of a Monte Carlo method. The calculated energy flux spectra lead to an escape flux phi(esc) about 6 x 10 to the 6th/sq cm per sec for Mars and phi(esc) about 2 x 10 to 6th/sq cm per sec for Titan, corresponding to a mass loss of about 0.14 kg/s for Mars and about 0.3 kg/s for Titan. (The contribution of electron impact ionization on N2 amounts to only about 25 percent of Titan's mass loss). Mass loss via solar and magnetospheric wind is also estimated using newly calculated mass loading limits. The mass loss via ion pickup from the extended hot atom corona for Mars amounts to about 0.25 kg/s (O/+/) and for Titan to about 50 g/s (N2/+/or H2CN/+/). Thus, the total mass loss rate from Mars and Titan is about the same (i.e., 0.4 kg/s).
Bauer Siegfried J.
Lammer Helmut
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