Suprathermal Ion Spectral Tails Throughout the Heliosphere: to 9 AU with Cassini, to 17 AU with New Horizons, and in the Outer Heliosphere and Heliosheath with Voyager 1 and 2

Details Suprathermal Ion Spectral Tails Throughout the Heliosphere: to 9 AU with Cassini, to 17 AU with New Horizons, and in the Outer Heliosphere and Heliosheath with Voyager 1 and 2 Suprathermal Ion Spectral Tails Throughout the Heliosphere: to 9 AU with Cassini, to 17 AU with New Horizons, and in the Outer Heliosphere and Heliosheath with Voyager 1 and 2

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh21a1793h&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH21A-1793

Physics

Plasma Physics

[2114] Interplanetary Physics / Energetic Particles, [2124] Interplanetary Physics / Heliopause And Solar Wind Termination, [2152] Interplanetary Physics / Pickup Ions, [7845] Space Plasma Physics / Particle Acceleration

Scientific paper

The shape of interplanetary suprathermal ion spectra, in particular the power law exponent, is of great interest in relation to the termination shock and heliosheath (e.g., due to the large influence of the suprathermal energy range in termination shock dynamics) and for acceleration and transport processes more generally (e.g., due to the heightened interest related to the Fisk and Gloeckler observations and theory of suprathermal tail formation). We have significant observational results on this issue from Cassini/CHEMS and the Voyager/LECP (the Charge Energy Mass Spectrometer and Low Energy Charged Particle experiments, respectively). New Horizons/PEPSSI (Pluto Energetic Particle Spectrometer Science Investigation) also has the capability to provide measurements in the suprathermal energy range. Like CHEMS, PEPSSI makes compositional measurements approximately above the pickup ion energy range. We report on the spatial and temporal variations of the suprathermal ion tail spectra at multiple spacecraft and characterize the phenomena of this important population across the heliosphere.

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