Latitudinal transport effects on the modulation of a few-MeV cosmic ray electrons from solar minimum to solar maximum

Details Latitudinal transport effects on the modulation of a few-MeV cosmic ray electrons from solar minimum to solar maximum Latitudinal transport effects on the modulation of a few-MeV cosmic ray electrons from solar minimum to solar maximum

Feb 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004jgra..10902115f&link_type=abstract

Journal of Geophysical Research, Volume 109, Issue A2, CiteID A02115

Astronomy and Astrophysics

Astrophysics

2

Solar Physics, Astrophysics, And Astronomy: Energetic Particles (2114), Solar Physics, Astrophysics, And Astronomy: Magnetic Fields, Solar Physics, Astrophysics, And Astronomy: Solar Activity Cycle (2162), Solar Physics, Astrophysics, And Astronomy: Solar And Stellar Variability, Solar Physics, Astrophysics, And Astronomy: Transition Region

Scientific paper

A three-dimensional, steady state, numerical model was used to model the propagation of 7 MeV jovian and galactic electrons in the heliosphere. The computations are compared with 3-10 MeV Ulysses/KET electron observations which are still not well explained after ~1998. To explain these observations, coinciding with solar maximum conditions, it is shown that a reduction in the enhancement of perpendicular transport toward the poles is required compared to solar minimum. The decrease in this enhancement can be correlated to the disappearance of the fast solar wind and/or a heliospheric magnetic field with a meridional component at solar maximum. By assuming a substantial jovian contribution to the total low-energy electron intensity at high latitudes to explain the Ulysses/KET observations in these regions, important information on the magnitude of perpendicular transport in the polar direction and its time dependence can be deduced.

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