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Fig. 1. | Earth, Planets and Space

Fig. 1.

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. 1.

Long-term variation of the amplitude D(j) and phase ϕ(j) of the solar diurnal variation D(j) of the neutrons and the vertical muon component observed at j stations, Inuvik (λ = 68°N, ϕ = 134°W; pc ∼ 0.2 GV), Apatity (68°N, 33°E; 0.7 GV), Hermanus (34°S, 19°E; 4.9 GV), Huancayo (12°S, 75° W; 13.0 GV) and Nagoya (V) (35°N, 137°E; 11.5 GV). P and N: the positive and negative states of the solar polar magnetic field.

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