Observations of Cosmic Rays and Solar Energetic Particles from the Ulysses COSPIN High Energy Telescope Following Completion of the Solar Maximum Solar Polar Passes.*

Details Observations of Cosmic Rays and Solar Energetic Particles from the Ulysses COSPIN High Energy Telescope Following Completion of the Solar Maximum Solar Polar Passes.* Observations of Cosmic Rays and Solar Energetic Particles from the Ulysses COSPIN High Energy Telescope Following Completion of the Solar Maximum Solar Polar Passes.*

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....6306m&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #6306

Physics

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At the end of 2002, following its second pass over the Sun's north polar region, Ulysses had reached a radial distance of about 4.5 AU at a heliographic latitude of 24°N. While solar activity remained high, the modulated intensity of cosmic rays observed by Ulysses’ COSPIN High Energy Telescope had increased significantly from the levels observed early in 2001, which most likely represented the maximum modulation for this solar cycle. Despite continuing solar activity, the new qA<0 magnetic polarity of the Sun's dipole field was fully established for both poles since the change in the North Pole polarity in 2000. Although the current sheet tilt was still large (>40° as reported by the Wilcox Solar Observatory) and the solar wind was still frequently disturbed by solar activity, it is worthwhile to examine the recent increase in the quiet-time cosmic ray fluxes for evidence of the change in latitudinal gradients expected upon change of magnetic polarity. A difficulty is the lack of a well-matched 1 AU base-line to help distinguish spatial from temporal variations following the termination of IMP-8 operations in late 2001. We will summarize Ulysses observations of energetic (>~30 MeV/n) protons and helium through the most recent available data, and will discuss available options for determining baseline fluxes at 1 AU for studies of the radial and latitudinal gradients. **This work was supported in part by NASA/JPL Contract 955432, by NASA Grant NASA 5-28516 and by NSF grant ATM 99-12341.

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