Proton Velocity Distributions in the Inner Heliosheath Derived from Energetic Hydrogen Atoms Measured with Cassini and IBEX

Details Proton Velocity Distributions in the Inner Heliosheath Derived from Energetic Hydrogen Atoms Measured with Cassini and IBEX Proton Velocity Distributions in the Inner Heliosheath Derived from Energetic Hydrogen Atoms Measured with Cassini and IBEX

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1302..110g&link_type=abstract

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

Astronomy and Astrophysics

Astrophysics

1

Pickups, Solar Wind, Spacecraft, Pickup Ions, Particle Emission, Solar Wind, Spacecraft/Atmosphere Interactions

Scientific paper

Recent definitive observations of Energetic Hydrogen Atoms (EHAs) with IBEX [1] and Cassini [2] allow us to deduce the proton velocity distribution in the region of EHA production. We consider four separate components: (a) the heliosheath (HS) solar wind, (b) HS pickup protons, (c) heliosphere pickup protons and (d) the -5 power law suprathermal tails that combine to produce the composite IBEX-LO, IBEX-HI and Cassini INCA EHA spectrum measured recently in the Voyager-1 direction (V-1). We find that (1) the current heliocentric distance of the heliopause (HP) along V-1, RHS, is 142-9+12, 148-9+12, and 158-9+12, AU using the interstellar neutral H density at the termination shock of 0.115, 0.100 and 0.085 cm-3, respectively, with the lower limits estimated using lower limits of the measured EHA differential intensities and assuming that ~30% of the EHAs come from outside the inner heliosheath; (2) the total particle pressure is (1.2+/-0.15)•10-12 dyne/cm2, remaining constant throughout the HS, although contributions from individual components vary with heliocentric distance from the termination shock (TS) (3) in order to explain the lowest energy published IBEX EHA flux, the amplitude of compressional turbulence is predicted to start increasing at (RHS-~10) AU, reaching (155+/-5) km/s and (4) near the HP, the -5 tail pressure rises, while the heliosphere pickup proton pressure falls. The Fisk and Gloeckler [3] model for ACR acceleration near the heliopause requires (3) and (4).

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