Survey of ion plasma parameters in Saturn's magnetosphere

Details Survey of ion plasma parameters in Saturn's magnetosphere Survey of ion plasma parameters in Saturn's magnetosphere

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010jgra..11510220t&link_type=abstract

Journal of Geophysical Research, Volume 115, Issue A10, CiteID A10220

Physics

24

Magnetospheric Physics: Planetary Magnetospheres (5443, 5737, 6033), Planetary Sciences: Fluid Planets: Magnetospheres (2756), Magnetospheric Physics: Plasma Sheet, Magnetospheric Physics: Plasmasphere, Magnetospheric Physics: Plasma Convection (2463)

Scientific paper

A survey of the bulk plasma ion properties observed by the Cassini Plasma Spectrometer instrument over roughly the first 4.5 years of its mission in orbit around Saturn is presented. The moments (density, temperature, and flow velocity) of the plasma distributions below 50 keV have been computed by numerical integration of the observed counts in the “Singles” (non-mass-resolved) data, partitioned into species on the basis of concurrent determinations of the composition from the time-of-flight data. Moments are presented for three main species: H+, W+ (water group ions), and ions with m/q = 2, which are presumed to be H2+. While the survey extends to radial distances of 30 RS and thus includes some solar wind or magnetosheath values, our principal interest is the large-scale spatial variation of the magnetospheric plasma properties, so we focus attention on radial distances inside of 17 RS. Principal findings include the following: (1) the densities of all three components are highly variable but are generally well organized by dipole L and magnetic latitude; (2) the density of ions with m/q = 2 varies from a few percentage of the H+ density in the inner magnetosphere to a maximum of several tens of percentage near the orbit of Titan, suggesting that Titan is an important source for H2+ in the outer magnetosphere; (3) water group ions are the dominant population in the inner magnetosphere, but only within ˜3 RS of the equatorial plane because of their strong centrifugal confinement; (4) derived latitudinal scale heights are largest for the light ions and generally increase with radial distance; (5) the L dependence of the calculated temperatures is not consistent with adiabatic transport but is in fair agreement with the expectations for plasma originating from ion pickup; (6) in agreement with the findings of Sergis et al. (2010), inside of L ˜ 11, the particle pressure is dominated by ions with energies below a few keV; (7) the derived flow velocities reveal the global circulation pattern of relatively dense populations in the magnetosphere, with no evidence for return circulation from the nightside to the dayside beyond ˜20 RS; and (8) the azimuthal flow speeds are typically less than full corotation over the entire L range examined, varying from ˜50% to 70% of full corotation.

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