Drifts and the Large Increase in the ACR Radial Gradients at Solar Maximum

Details Drifts and the Large Increase in the ACR Radial Gradients at Solar Maximum Drifts and the Large Increase in the ACR Radial Gradients at Solar Maximum

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh52b..09j&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH52B-09

Other

7859 Transport Processes, 2104 Cosmic Rays, 2114 Energetic Particles, Heliospheric (7514), 2134 Interplanetary Magnetic Fields, 2162 Solar Cycle Variations (7536)

Scientific paper

We have investigated the physical mechanism responsible for the observed large (factor of 10) change in the radial gradient of anomalous cosmic rays observed in the outer heliosphere near the recent maximum in solar activity. The increase in gradient and corresponding decrease in intensity occurred even in the absence of large disturbances or other significant transient phenomena in the solar wind. However, it did occur during a period where the magnetic configuration at the Sun was changing rapidly. The Arizona three-dimensional cosmic-ray modulation model has been extended to include a dynamically changing current sheet in a fully time-dependent code, which includes the complete three-dimensional, time-varying magnetic field. We considered a simple heliosphere model in which the tilt of the current sheet changed continuously through a full 360 degrees in 22 years. This could be a crude simulation of the solar magnetic cycle, where the magnetic-field orientation change at sunspot maximum simply corresponds to the tilt angle passing through 90 or 270 degrees. To isolate the effects, no other parameter was changed. Preliminary results from this model show encouraging similarity to the anomalous-cosmic-ray observations near solar maximum. The physics of this model and the relation to observations will be discussed.

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