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Annales Geophysicae An interactive open-access journal of the European Geosciences Union
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Volume 21, issue 6
Ann. Geophys., 21, 1359–1366, 2003
https://doi.org/10.5194/angeo-21-1359-2003
© Author(s) 2003. This work is distributed under
the Creative Commons Attribution 3.0 License.

Special issue: Ulysses and Beyond

Ann. Geophys., 21, 1359–1366, 2003
https://doi.org/10.5194/angeo-21-1359-2003
© Author(s) 2003. This work is distributed under
the Creative Commons Attribution 3.0 License.

  30 Jun 2003

30 Jun 2003

Charge-sign dependent modulation in the heliosphere over a 22-year cycle

S. E. S. Ferreira1,3, M. S. Potgieter1, B. Heber2, and H. Fichtner3 S. E. S. Ferreira et al.
  • 1Unit for Space Physics, School of Physics, Potchefstroom University for CHE, 2520 Potchefstroom, South Africa
  • 2Fachbereich Physik, Universität Osnabrück, 49069 Osnabrück, Germany
  • 3Institut für Theoretische Physik, Lehrstuhl IV: Weltraum und Astrophysik, Ruhr-Universität Bochum, Germany

Abstract. A time-dependent model based on a numerical solution of Parker’s transport equation is used to model the modulation of cosmic ray protons, electrons and helium for full 11-year and 22-year modulation cycles using a compound approach. This approach incorporates the concept of propagating diffusion barriers based on global increases in the heliospheric magnetic field as they propagate from the Sun throughout the heliosphere, combined with gradient, curvature and current sheet drifts and the other basic modulation mechanisms. The model results are compared to the observed 11-year and 22-year cycles for 1.2 GV electrons and 1.2 GV Helium at Earth for the period 1975–1998. The model solutions are also compared to the observed charge-sign dependent modulation along Ulysses’ trajectory for the period 1990–1998. This compound approach to long-term modulation, especially charge-sign dependent modulation, is found to be remarkably successful. It is shown that the model can easily account for the latitude dependence for cosmic ray protons and the lack thereof for cosmic ray electrons by assuming large perpendicular diffusion in the polar direction. This approach contributes to an improved understanding of how diffusion and drifts vary from solar minimum to maximum modulation, and what the time-dependence of the heliospheric diffusion coefficients may be.

Key words. Interplanetary physics (energetic particles; cosmic rays; general or miscellaneous)

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