ENA (E>5 keV) Images from Cassini and Voyager ``ground truth'': Suprathermal Pressure in the Heliosheath

Details ENA (E>5 keV) Images from Cassini and Voyager ``ground truth'': Suprathermal Pressure in the Heliosheath ENA (E>5 keV) Images from Cassini and Voyager ``ground truth'': Suprathermal Pressure in the Heliosheath

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1302...79k&link_type=abstract

PICKUP IONS THROUGHOUT THE HELIOSPHERE AND BEYOND: Proceedings of the 9th Annual International Astrophysics Conference. AIP Con

Astronomy and Astrophysics

Astrophysics

4

Solar Wind, Spacecraft, Pickups, Interstellar Matter, Particle Emission, Solar Wind, Spacecraft/Atmosphere Interactions, Pickup Ions, Interstellar Dust Grains, Diffuse Emission, Infrared Cirrus

Scientific paper

Maps of energetic neutral atoms (ENA) of the heliosphere from Cassini [1] have been constructed spanning the energy range ~5<=E<=55 keV, and show a ``Belt'' in the sky of ~100° FWHM. Similarly, maps >6 keV have been obtained by the IBEX mission [2] and show a ``Ribbon'' that is narrower than the Belt and inclined to it in both ecliptic latitude (~25°) and longitude (~30°). The overlap in energy between Voyager ions [3] and Cassini ENA intensities (averaged over the ENA line of sight) enables us to deduce ion fluxes in the heliosheath, thus providing a continuous spectrum 5<=E<=4000 keV. These measurements are then used to estimate the local partial pressure over this energy range (~0.1 pPa), suggesting β>25 [4] and the thickness of the heliosheath (~50 AU). Using a simulated PUI distribution [5], we estimate the E<6 keV contribution to be ~0.12 pPa. The balance of the non-thermal pickup ion (PUI) pressure against the stagnation pressure of the interstellar plasma and the local interstellar magnetic field (ISMF) at the nose of the heliopause implies an upper bound on the ISMF of ~0.64 nT.

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