The Ulysses fast latitude scan at solar maximum: COSPIN/KET observations

Details The Ulysses fast latitude scan at solar maximum: COSPIN/KET observations The Ulysses fast latitude scan at solar maximum: COSPIN/KET observations

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh22a0744h&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH22A-0744

Other

2104 Cosmic Rays, 2114 Energetic Particles, Heliospheric (7514), 2118 Energetic Particles, Solar

Scientific paper

Ulysses, launched in October 1990, began in December 1997 its second out of ecliptic orbit, and in September 2000 its second fast latitude scan. In contrast to the first fast latitude scan in 1994/1995 solar activity is close to maximum. It is important to note, that in addition to the different solar activity levels the solar magnetic field had reversed in 2000. While the first latitude scan gave a snapshot of the spatial distribution of galactic cosmic rays the second one is determined by temporal variations. Solar particle increases are observed at all heliographic latitudes, including events producing >250~MeV protons and ~50~MeV electrons. Sources of MeV electrons in the inner heliosphere are 1) solar energetic particle events, 2) galactic cosmic rays, and 3) Jupiter. Since the first population is generally accompanied by energetic nucleons they can be distinguished from the other components by investigating e.g.~34-69~MeV protons. We found ``quiet time'' increases at all heliospheric latitudes, which indicate either very large perpendicular diffusion or the possibility of direct magnetic connection from low latitudes to polar regions. Concerning galactic cosmic ray modulation, we will compare the latitudinal gradient as well as the charge sign dependent variation for both Ulysses fast latitude scans.

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