Cosmic Ray Transport in a Heliospheric Magnetic Field with Non-Polar Coronal Holes

Details Cosmic Ray Transport in a Heliospheric Magnetic Field with Non-Polar Coronal Holes Cosmic Ray Transport in a Heliospheric Magnetic Field with Non-Polar Coronal Holes

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001ssrv...97..327k&link_type=abstract

Space Science Reviews, v. 97, Issue 1/4, p. 327-330 (2001).

Computer Science

3

Scientific paper

The simple tilted dipole picture of Corotating Interaction Regions which prevailed during the first polar pass of Ulysses no longer applies since the Sun entered a more active phase. Recent observations show that CIRs still persist, though the large polar coronal holes of solar minimum shrink to smaller areas and move to lower latitudes. We present 3-D simulations for the cosmic-ray intensity variations in a model with non-polar high speed streams. Latitudinal and recurrent time-variations are discussed, but more detailed and realistic simulations are required before quantitative comparisons with observations can be made.

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