Modelling cosmic ray intensities along the Ulysses trajectory

Autor(en): Ndiitwani, DC
Ferreira, SES
Potgieter, MS
Heber, B
Stichwörter: Astronomy & Astrophysics; cosmic rays; DIFFUSION TENSOR; DRIFT MODEL; ELECTRONS; energetic particles; Geology; Geosciences, Multidisciplinary; HELIOSPHERIC MAGNETIC-FIELD; interplanetary physics; magnetic fields; MERGED INTERACTION REGIONS; Meteorology & Atmospheric Sciences; PERSPECTIVE; SIMULATION; solar physics, astrophysics and astronomy; SOLAR-WIND; TIME-DEPENDENT MODULATION; TRANSPORT
Erscheinungsdatum: 2005
Volumen: 23
Ausgabe: 3
Startseite: 1061
Seitenende: 1070
Time dependent cosmic ray modulation in the inner heliosphere is studied by comparing results from a 2-D, time-dependent cosmic ray transport model with Ulysses observations. A compound approach, which combines the effects of the global changes in the heliospheric magnetic field magnitude with drifts to establish a realistic time-dependence, in the diffusion and drift coefficients, are used. We show that this model results in realistic cosmic ray modulation from the Ulysses launch (1990) until recently (2004) when compared to 2.5-GV electron and proton and 1.2-GV electron and Helium observations from this spacecraft. This approach is also applied to compute radial gradients present in 2.5-GV cosmic ray electron and protons in the inner heliosphere. The observed latitude dependence for both positive and negative charged particles during both the fast latitude scan periods, corresponding to different solar activity conditions, could also be realistically computed. For this an additional reduction in particle drifts (compared to diffusion) toward solar maximum is needed. This results in a realistic charge-sign dependent modulation at solar maximum and the model is also applied to predict charge-sign dependent modulation up to the next expected solar minimum.
ISSN: 09927689
DOI: 10.5194/angeo-23-1061-2005

Show full item record

Google ScholarTM