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Voyager Results Revisited

Voyager Results Revisited. By Ed Sittler NASA/GSFC CAPS Team Meeting #28 Marseille, France July 26-28, 2004. Voyager Encounter Geometry. Saturn Encounter Trajectories. Saturn’s Magnetospheric Plasma. Voyager 1 Plasma Electrons. Voyager 2 Plasma Electrons. Voyager 1 Electron Spectrum.

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Voyager Results Revisited

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  1. Voyager Results Revisited By Ed Sittler NASA/GSFC CAPS Team Meeting #28 Marseille, France July 26-28, 2004

  2. Voyager Encounter Geometry

  3. Saturn Encounter Trajectories

  4. Saturn’s Magnetospheric Plasma

  5. Voyager 1 Plasma Electrons

  6. Voyager 2 Plasma Electrons

  7. Voyager 1 Electron Spectrum

  8. Voyager 2 Electron Spectrum

  9. Voyager Ion Measurements

  10. Voyager 1 Ions at Ring Plane

  11. Saturn’s Radiation Belts

  12. Saturn’s Ring Current

  13. Saturn’s Outer Magnetosphere

  14. Saturn’s Outer Magnetosphere Energetic Ion and Electron Events

  15. OH Cloud with Saturn’s Inner Magnetosphere (HST Observations)

  16. Titan’s Nitrogen Torus

  17. Enrichment of Nitrogen Ion’s within Saturn’s Inner Magnetosphere? • Solar wind source of keV protons and alphas • Titan Torus as source of keV Nitrogen Ions • Ions energized as they diffuse inward to form radiation belts within inner magnetosphere. • Radial diffusion and Convection • Charged particle sinks • Wave scattering by MHD waves • Satellite sweeping • Loss due to dust particles • Charge exchange losses with neutral clouds

  18. 800 keV Electrons Starting at L = 7 Static Solar Wind (V = 400 km/s) Dawn Dusk

  19. Energy Spectrum of Ions and Electrons within Titan’s Neutral Torus

  20. Satellite Sweeping by Rhea

  21. Energy Spectrum of Ions and Electrons at Dione’s L Shell

  22. Summary • Voyager plasma data showed presence of light ion component (H+) and heavy ion component (N+,O+,W+). Did not see evidence of H2+. • Data consistent with heavy ions dominating near equator and light ions dominating at high latitudes. • Electron observations show plasma sheet within inner magnetosphere inside L ~ 15 and time dependent region in outer magnetosphere. • Electron data shows keV electrons confined near equatorial plane (T/Tll >> 1). Same is true for energetic electrons (LECP). • Expect energetic heavy ions to be confined to equatorial plane, while protons more isotropic and at all latitudes (LECP). • PLS observed hot keV ion component (N+/O+) confined to equatorial plane in Titan torus region (T/Tll >> 1). Hot keV ion component (N+, O+, W+) also observed at Dione’s L shell ring plane crossing. • Ions typically sub-corotate in outer magnetosphere at ~ 50% of co-rotation. Ionospheric pederson height conductivity ~ 0.2 mho. • Saturn’s magnetosphere falls in the category of a fast rotator where neutral clouds can dominate the plasma environment by number.

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