Energetic particle pressure in Saturn's magnetosphere measured with the Magnetospheric Imaging Instrument on Cassini

Details Energetic particle pressure in Saturn's magnetosphere measured with the Magnetospheric Imaging Instrument on Cassini Energetic particle pressure in Saturn's magnetosphere measured with the Magnetospheric Imaging Instrument on Cassini

Feb 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009jgra..11402214s&link_type=abstract

Journal of Geophysical Research, Volume 114, Issue A2, CiteID A02214

Physics

Plasma Physics

23

Planetary Sciences: Fluid Planets: Magnetospheres (2756), Planetary Sciences: Solar System Objects: Saturn, Planetary Sciences: Fluid Planets: Interactions With Particles And Fields, Space Plasma Physics: Neutral Particles (2151), Planetary Sciences: Fluid Planets: General Or Miscellaneous

Scientific paper

The Magnetospheric Imaging Instrument on board Cassini has been providing measurements of energetic ion intensities, energy spectra, and ion composition, combining the Charge Energy Mass Spectrometer over the range 3 to 236 keV/e, the Low Energy Magnetospheric Measurements System for ions in the range 0.024 to 18 MeV, and the Ion and Neutral Camera for ions and energetic neutral atoms in the range 3 to > 200 keV. Results of the energetic (E > 3 keV) particle pressure distribution throughout the Saturnian magnetosphere and comparison with in situ measurements of the magnetic pressure are presented. The study offers a comprehensive depiction of the average, steady state hot plasma environment of Saturn over the 3 years since orbit insertion on 1 July 2004, with emphasis on ring current characteristics. The results may be summarized as follows: (1) The Saturnian magnetosphere possesses a dynamic, high-beta ring current located approximately between 8 and ~15 RS, primarily composed of O+ ions, and characterized by suprathermal (E > 3 keV) particle pressure, with typical values of 10-9 dyne/cm2. (2) The planetary plasma sheet shows significant asymmetries, with the dayside region being broadened in latitude (+/-50°) and extending to the magnetopause, and the nightside appearing well confined, with a thickness of ~10 RS and a northward tilt of some 10° with respect to the equatorial plane beyond ~20 RS. (3) The average radial suprathermal pressure gradient appears sufficient to modify the radial force balance and subsequently the azimuthal currents. (4) The magnetic perturbation due to the trapped energetic particle population is ~7 nT, similar to values from magnetic field-based studies (9 to 13 nT).

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