Physics – Plasma Physics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsm23c1637e&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #SM23C-1637
Physics
Plasma Physics
[0343] Atmospheric Composition And Structure / Planetary Atmospheres, [6265] Planetary Sciences: Solar System Objects / Planetary Rings, [7823] Space Plasma Physics / Ionization Processes, [7837] Space Plasma Physics / Neutral Particles
Scientific paper
The primary source of neutral O2 for Saturn’s magnetosphere is due to solar UV photons protons that produce O2 from H2O ice decomposition over the main rings as well as the tenuous F and G rings resulting in a tenuous O2 atmosphere (Johnson et. al. 2006). The O2 atmosphere is very thin to the point of being nearly collisionless. Our model of the atmosphere predict that as it interacts with the ring particles, the O2 is adsorbed and desorbed from the rings causing changes in the trajectories, which in turn, allows for a distribution of O2 from the rings throughout the magnetosphere (Tokar et. al. 2005; Tseng et. al. 2009). Predominately through photo-ionization and ion-exchange these O2 neutrals from the ice grains become a source for O2+ ions in the inner magnetosphere. Once the O2 becomes ionized to become O2+ the ions then follow the field lines. The ions interact with the ice particles in the rings to stick to the ring particles effectively reducing the ion density. As a result the ion density is greater over the Cassini Division and the area between the F and G ring where the optical depth due to the ice grain is less. Accordingly, the neutral O2 densities would tend to be high over the higher optical depth of the B and A main rings where the source rates are higher. Models of the neutral densities have shown high densities over the main rings, with a tail through the magnetosphere. Analysis of the CAPS (Cassini Plasma Spectrometer) data from the Saturn Orbit Insertion (SOI) in 2004 shows a peak in density over the Cassini Division and a higher peak in O2+ ion density between the F and G rings. References: Johnson, R.E., J.G. Luhmann, R.L. Tokar, M. Bouhram, J.J. Berthelier, E.C. Siler, J.F. Cooper, T.W. Hill, H.T. Smith, M. Michael, M. Liu, F.J. Crary, D.T. Young, "Production, Ionization and Redistribution of O2 Saturn's Ring Atmosphere" Icarus 180, 393-402 (2006).(pdf) Tokar, R.L., and 12 colleagues, 2005. Cassini Observations of the Thermal Plasma in the Vicinity of Saturn’s Main Rings and the F and G Rings. Geophys. Res. Lett. 32, doi:10.1029/2005GL022690. L14S04. Martens, H. R., Reisenfeld, D. B., Williams, J. D., Johnson, R.E., Smith H. T., “Observations of molecular oxygen ions in Saturn’s inner magnetosphere”. Geophy. Res. Lett. 2009. W.-L. Tseng, Ip, W.-H., Johnson, R. E., Cassidy, T. A., Elrod, M. K., “The Structure and Time Variability of the Ring atmosphere and ionosphere”. Geophy. Res. Lett. 2009.
Cassidy Timothy A.
Elrod Meredith K.
Ip Wing
Johnson Robert E.
Tseng W.
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