Voyager Observation of Galactic Cosmic Ray Elctrons in the Heliosheath

Details Voyager Observation of Galactic Cosmic Ray Elctrons in the Heliosheath Voyager Observation of Galactic Cosmic Ray Elctrons in the Heliosheath

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh11a..08m&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH11A-08

Physics

2104 Cosmic Rays, 2114 Energetic Particles (7514), 2124 Heliopause And Solar Wind Termination

Scientific paper

Voyager 1 observations of low-energy, (2.5-140 MeV), highly relativistic, galactic cosmic ray (GCR) electrons are important in studying the transport of energetic particles and the nature of transient disturbances in the heliosheath. These electrons originate as directly accelerated primaries, as interstellar secondaries from the decay of charged pions, or at low energies as knock-on electrons produced by the passage of higher energy cosmic rays through the interstellar medium. Inside 10 AU below some 60 MeV, Jovian electrons are the dominant electron component. Except for solar (out to 30 AU) and Jovian electrons there was no increase in the electron channels above the background level until V1 approached the termination shock in mid 2002. Since crossing the termination shock there has been a strong increase in the electron intensity with radial gradients of 6 - 75 MeV electrons that are inferred to be on the order of 18%/AU. The 10 MeV component appears to be especially sensitive to the passage of transient disturbances through the heliosheath. As V2 began observing an extended termination shock particle event in late 2004 there have been accompanying increases of 2.5 - 14 MeV electrons that are probably related to the interaction between interplanetary disturbances, the termination shock and the existing GCR electrons.

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