Evolution of the Energy Spectra of Low-Energy Particles at Voyagers 1 and 2 in the Outer Heliosphere and Implications for the Source Location of Anomalous Cosmic Rays

Details Evolution of the Energy Spectra of Low-Energy Particles at Voyagers 1 and 2 in the Outer Heliosphere and Implications for the Source Location of Anomalous Cosmic Rays Evolution of the Energy Spectra of Low-Energy Particles at Voyagers 1 and 2 in the Outer Heliosphere and Implications for the Source Location of Anomalous Cosmic Rays

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh11a..06c&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH11A-06

Physics

2104 Cosmic Rays, 2114 Energetic Particles (7514), 2124 Heliopause And Solar Wind Termination, 2126 Heliosphere/Interstellar Medium Interactions

Scientific paper

As of this writing, 4 September 2007, the Voyager 1 (V1) spacecraft is at 103.8 AU and 34.3 deg N. It is in the heliosheath, presumably about 10 AU beyond the solar wind termination shock. The Voyager 2 (V2) spacecraft is at 83.7 AU and 27.5 deg S. It has not crossed the termination shock but may be close, having been observing low-energy termination shock particles since ~2005.0. In addition, very recently the intensity of protons with ~2-8 MeV at V2 has grown to exceed that at V1 by a factor of ~3. From ~10 to 100 MeV, the V2 intensity is lower than that at V1. For He, from ~10-25 MeV/nuc, the V2 energy spectrum is below that of V1 but well above that at V1 when it crossed the shock in late 2004. Energy spectra at both spacecraft have recently been evolving. The spectral observations at V2 when it crosses the termination shock compared to the spectra at V1 at the same time and at the time V1 crossed may help determine the source location of the anomalous cosmic rays. Finally, the energy spectra of H and O scale to that of He with multiplicative factors in energy/nucleon and intensity that suggest that the diffusion coefficient is proportional to particle speed times rigidity to the power ~1.4. This work was supported by NASA under contract NAS7-03001.

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