Daytime Pc 3–4 pulsation activities observed at globally coordinated low-latitude stations [SGC (L = 1.8, λ = 118.0°W), EWA(1.15,158.1°W), ONW(1.3,141.5°E)] are evidently controlled by the cone angle θ XB of the IMF observed at ISEE 3. Moreover, the Pc 3–4 frequencies ( ƒ) at the low latitudes and high latitude (COL; L = 5.6 and λ = 147.9°W) on the ground and that of compressional waves at geosynchronous orbit ( GOES 2; L = 6.67 and λ = 106.7°W) are also correlated with the IMFmagnitude( B IMF).The correlation of ƒ of the compressional Pc 3–4 waves at GOES 2 against B IMF is higher than those of the Pc 3–4 pulsations at the globally coordinated ground stations, i.e., γ = 0.70 at GOES 2, and (0.36,0.60,0.66,0.54) at (COL, SGC, EWA, ONW), respectively. The standard deviation ( σ n = ± Δƒ mHz ) of the observed frequencies from the form ƒ (mHz) = 6.0 × B IMF (nT) is larger at the ground stations than at GOES 2, i.e., Δƒ = ± 6.6 mHz at GOES 2, and ±(13.9, 9.1, 10.7, 12.1) mHz at (COL, SGC, EWA, ONW), respectively. The correlations between the IMF magnitude B IMF and Pc 3–4 frequencies at the low latitudes are higher than that at the high latitude on the ground, which can be interpreted by a “filtering action” of the magnetosphere for daytime Pc 3–4 magnetic pulsations. The scatter plots of pulsation frequency ƒ against the IMF magnitude B IMF for the compressional Pc 3–4 waves at GOES 2 are restricted within the forms ƒ = 4.5 × B IMF and ƒ = 7.5 × B IMF . The frequency distribution is in excellent agreement with the speculation ( <ω sc Ω i = 0.3 ∼ 0.5 ) of the spacecraft frame frequency of the magnetosonic right-hand waves excited by the anomalous ion cyclotron resonance with reflected ion beams with V ‖ = 650 ∼ 1150 km s −1 in the solar wind frame observed by the ISEE satellite in the Earth's foreshock. These observational results suggest that the magnetosonic right-handed waves excited by the reflected ion beams in the Earth's foreshock are convected through the magnetosheath to the magnetopause, transmitted into the magnetosphere without significant changes in spectra, and then couple with various HM waves in the Pc 3–4 frequency range at various locations in the magnetosphere.