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Fig. 5. | Earth, Planets and Space

Fig. 5.

From: The influence of the sidereal cosmic-ray anisotropies originated on the tail- and nose-boundaries of the heliomagnetosphere (HMS) upon the solar cosmic-ray anisotropy produced inside the HMS

Fig. 5.

-diagram showing the distributions of D(Herm) at Hermanus (34°S, 19°E; 4.9 GV) during the period (1965–2000) on the left and D(V) at Nagoya (35°N, 137°E; 11.5 GV) during the period (1971–2000) on the right. in the net area can be explained by the solar anisotropy with the parameter γ and pu at the point. The number attached each point expresses the observation year in the 1970s and 1990s in the P-state.

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