The Approach to Solar Maximum Conditions in the Outer Heliosphere as Seen in Anomalous Cosmic Rays

Details The Approach to Solar Maximum Conditions in the Outer Heliosphere as Seen in Anomalous Cosmic Rays The Approach to Solar Maximum Conditions in the Outer Heliosphere as Seen in Anomalous Cosmic Rays

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh22f08c&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH22F-08

Physics

2104 Cosmic Rays, 2114 Energetic Particles, Heliospheric (7514), 2124 Heliopause And Solar Wind Termination, 2162 Solar Cycle Variations (7536)

Scientific paper

The intensity of anomalous cosmic ray (ACR) protons and helium nuclei at the energy of the peak intensity of their spectrum began to level off in 1998 from their steady increase following the 1990 solar maximum period. In 1999, the intensities began to decline, signalling the onset of a new period of solar maximum conditions in the outer heliosphere. By 1 June 2001, the Voyager 1 (V1) spacecraft will be at 81 AU from the Sun and at a latitude of 33 degrees North. Voyager 2 (V2) will be at 64 AU and located 23 degrees South of the heliographic equator. Voyager 1 is entering the range of recent estimates of the location of the solar wind termination shock ( ~85 AU), where we expect to see the maximum intensities of ACRs. At the same time, solar maximum conditions are permeating the entire heliosphere, which would lead to reduced intensities. In addition, the Sun's magnetic field is in the process of reversing and the resulting complex field topology is propagating towards the outer heliosphere. We will compare the time-history profiles of ACR intensities at V1 and V2 during this approach to solar maximum and attempt to infer clues to the location of the solar wind termination shock. This work was supported by NASA under contract NAS7-918.

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