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-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.Back to article page