Other
Scientific paper
Dec 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh41b..01s&link_type=abstract
American Geophysical Union, Fall Meeting 2004, abstract #SH41B-01
Other
2104 Cosmic Rays, 2114 Energetic Particles, Heliospheric (7514), 2124 Heliopause And Solar Wind Termination, 2134 Interplanetary Magnetic Fields
Scientific paper
For most of the last two and a half years, Voyager 1 has observed enhanced intensities of energetic ions streaming along the magnetic field, suggesting that the source is a durable rather than transient feature of this region of the heliosphere beyond 85 AU. If Voyager 1 is in the solar wind, the beaming requires a non-spherical termination shock, but is the asymmetry of the shock large enough and in the right location? The small average radial anisotropy requires a large radial gradient, but is that consistent with lack of energy dependent modulation at low energies? If Voyager 1 is in the heliosheath, the outward beaming direction and small radial anisotropy are consistent, but are strong, persistent beams expected in the turbulent heliosheath, and what is the mechanism for avoiding the expected compression of the magnetic field? Whether or not Voyager 1 crossed the shock, there appear to be two distinct sources of accelerated interstellar pickup ions. Why does the nearby source region connected directly to Voyager 1 accelerate He ions to less that ~10 MeV/nucleon, while the more distant source region accelerates He ions to much higher energies? These and other aspects of the observations are revealing the unexpected nature of the termination shock and particle acceleration.
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