The Local Interstellar Spectrum Beyond the Heliopause: What can be Learned from Voyager in the Inner Heliosheath

Details The Local Interstellar Spectrum Beyond the Heliopause: What can be Learned from Voyager in the Inner Heliosheath The Local Interstellar Spectrum Beyond the Heliopause: What can be Learned from Voyager in the Inner Heliosheath

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh11a1914k&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH11A-1914

Physics

[2104] Interplanetary Physics / Cosmic Rays, [2114] Interplanetary Physics / Energetic Particles, [2124] Interplanetary Physics / Heliopause And Solar Wind Termination

Scientific paper

The expanding solar wind interacts with the local interstellar medium, resulting in the formation of the heliosphere. This interaction leads to three discontinuities the innermost one of which, the termination shock, has been explored by the two Voyager spacecraft. These spacecraft are now on their way to the second discontinuity, the heliopause, the region which separates the solar wind from the local interstellar medium. Further out a third discontinuity presumably exists, a bow shock in front of the heliosphere. The Voyager measurements clearly reveal that galactic cosmic rays are modulated in the inner heliosheath, the region between termination shock and heliopause as well. In addition Scherer et al. (2011) recently showed by means of numerical simulations that galactic cosmic rays, in contrast to previous assumptions, occur modulated in the outer heliosheath as well, i.e. the region between heliopause and bow shock. A consequence of this is that the local interstellar spectrum (LIS) can not be determined from the Voyager measurements unambiguously, but the recent estimates of the spectrum by Webber & Higbie (2009) can be used instead as the heliopause spectrum. Using this heliopause spectrum as well as the results by Scherer et al. (2011) we will show that the diffusion coefficient is consistent with 1e27 cm^2/s when using the LIS model by Webber & Higbie (2003). By restricting the analysis to the energy-range of 0.4 to 8 GeV, which is most important for the atmospheric production of the cosmogenic radionuclide 10Be, we show that the diffusion coefficient varies most likely in the range of 1e26 to 1e27 cm^2/s depending on the proposed LIS model.

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