Transverse cosmic ray gradients in the heliosphere and the solar diurnal anisotropy

Details Transverse cosmic ray gradients in the heliosphere and the solar diurnal anisotropy Transverse cosmic ray gradients in the heliosphere and the solar diurnal anisotropy

Aug 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997jgr...10217433a&link_type=abstract

Journal of Geophysical Research, Volume 102, Issue A8, p. 17433-17444

Physics

Plasma Physics

18

Interplanetary Physics: Cosmic Rays, Interplanetary Physics: Interplanetary Magnetic Fields, Interplanetary Physics: Solar Wind Plasma, Space Plasma Physics: Charged Particle Motion And Acceleration

Scientific paper

We describe a new scheme for computing the asymmetric part of the cosmic ray particle density gradient. The method makes use of the ecliptic components (Ar,Aϕ) of the cosmic ray solar diurnal anisotropy observed with a detector on spinning Earth and the interplanetary magnetic field sector structure in the heliosphere. We apply this methodology, to compute the magnitudes and directions of the asymmetric (Gθa) particle density gradient in the heliosphere for selected intervals of time during the 1965 to 1993 period. Data from six detectors of the global network are used for this purpose. Their median rigidity of response (Rm) covers the following range: 10GV<=Rm<=300GV of the galactic cosmic ray (GCR) spectrum. We find that Gθa is well behaved over an intermediate rigidity range (10GV<=Rm<=67GV) where it is inversely proportional to the rigidity (R) of the GCR protons. At higher rigidities (R>=100GV), it may fall off more steeply and even reverse sign at large (>~1AU) off-ecliptic distances. The direction of Gθa changes consistently immediately after each observed solar polar field reversal. Sudden, conspicuous, short-lived (~1 year) reversals of Gθa are observed during the declining phases of solar activity cycles 20 (1974) and 21 (1984). They may be caused by a sudden burst of solar activity late in the cycle. We have determined Gθa values from Deep River neutron monitor data (Rm=16GV) for the 1965 to 1993 period. Extreme computed values range from (3.0+/-0.8)%/AU in 1968 to (-2.4+/-0.8)%/AU in 1987.

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