Voyager Studies of Cosmic Ray Transport in the Heliosheath

Details Voyager Studies of Cosmic Ray Transport in the Heliosheath Voyager Studies of Cosmic Ray Transport in the Heliosheath

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh51b1674m&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH51B-1674

Physics

[2104] Interplanetary Physics / Cosmic Rays

Scientific paper

V1 crossed the termination shock on 2004.96 [94 AU, 36°N] and has moved at least 20 AU deeper into the heliosheath over the last 6 years. This period spans the time from the end of solar maximum modulation conditions in the distant heliosphere to those of the current deep solar minimum conditions of cycle 23/24. V2 crossed into the heliosheath on 2007.66 (83.7AU, 26°S). Despite their physical separation of ~ 115 AU and 45° in heliolongitude, there is a close correspondence of the GCR H and He intensity >175 MeV/n, higher energy ACR He (> 30 MeV/n) and 2.5 MeV H termination shock particles between the two spacecraft. Over most of this period (starting in 2004.9) the instantaneous radial gradient of 265 MeV/n H and He has been ~ 0.2 ‡ 0.2%/AU except for a period beginning in 2009.15 when most particle intensities at V2 experienced an unexplained small decrease while continuing to increase at V1. The small radial gradients suggest that these intensity increases are mainly temporal and not spatial. For GCR carbon >30 MeV/n, the spectral slope is proportional to the kinetic energy - a characteristic of particles that have been adiabatically cooled in the supersonic solar wind. The largest changes are found for 2.5 - 160 MeV electrons with 10 MeV electrons increasing at an average rate of 75%/year. There is a significant difference between the electron time histories at V1 and V2. These initial GCR observations establish that the heliosheath plays a major role in the modulation process in a manner that was not generally envisioned in the past.

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