A numerical model for a cosmic ray modulation barrier in the outer heliosphere

Details A numerical model for a cosmic ray modulation barrier in the outer heliosphere A numerical model for a cosmic ray modulation barrier in the outer heliosphere

Jan 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...209..406p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 209, no. 1-2, Jan. 1989, p. 406-410.

Astronomy and Astrophysics

Astrophysics

18

Cosmic Rays, Heliosphere, Interplanetary Medium, Solar Activity Effects, Interplanetary Magnetic Fields, Modulation, Protons, Solar Cycles, Time Dependence

Scientific paper

Current steady-state, cosmic-ray modulation models, with and without drift, have difficulties explaining the observed constant interplanetary radial gradient for the period 1977-1982. To explain this constancy it has recently been proposed that most of solar modulation occurs in a modulation barrier which surrounds the heliosphere. Following this argument, the effect of such a barrier located in the outer heliosphere and declining (or extending) with time was investigated using a time-dependent, spherically-symmetric model. Despite a factor of 3 increase in the 1.5 GeV proton intensity at earth caused by the declining barrier, the radial gradient remained between 2.8-3.6 percent per AU, almost independent of radial distance and time. Under similar circumstances a conventional model produces a factor of 3 change in the radial gradient. The concept of an outer heliospheric modulation barrier, which respectively expands and contracts with increasing and decreasing solar activity, can therefore in principle produce an 11 year modulation cycle.

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