Out-of-ecliptic quiet time MeV electron increases: Ulysses COSPIN/KET observations

Details Out-of-ecliptic quiet time MeV electron increases: Ulysses COSPIN/KET observations Out-of-ecliptic quiet time MeV electron increases: Ulysses COSPIN/KET observations

Apr 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aipc..703..157h&link_type=abstract

PLASMAS IN THE LABORATORY AND IN THE UNIVERSE: New Insights and New Challenges. AIP Conference Proceedings, Volume 703, pp. 157

Physics

Particle Emission, Solar Wind, Magnetohydrodynamics And Plasmas

Scientific paper

The propagation of cosmic rays in turbulent magnetic fields can be studied in detail by way of in-situ measurements of energetic particles in the three-dimensional heliosphere. Measurements of 3-20 MeV electrons from 1990 to 2003 have been made by the Kiel Electron Telescope (KET) onboard the Ulysses spacecraft during varying solar conditions. In order to interpret these measurements, it is necessary to distinguish between solar, galactic and Jovian electrons and to investigate their propagation, by using sophisticated particle propagation models. The solar contribution to the MeV electron intensities can be excluded by analyzing the electron energy spectra and the nuclei time histories. The residual electron intensities can be reasonably described by modulation models taking into account galactic cosmic rays as well as Jovian electrons using different diffusion coefficients for solar minimum and maximum. The way in which the relative contribution of Jovian (point source in the ecliptic) and galactic electrons (isotropic source) varies along the Ulysses orbit is strongly dependent on the choice of these coefficients. Since the 1970's quiet time electron increases have been observed in the ecliptic and interpreted as Jovian electron increases. Therefore, the occurrence of such quiet time electron increases is an indicator for a dominant Jovian contribution to the measured MeV electron intensities. At solar minimum and maximum such events have been observed up to ~30°and ~45°. These observations are crucial for a determination of the diffusion parameters. At solar maximum a more efficient latitude transport is needed to account for the electron intensity variations.

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