The paper discusses a magnetohydrodynamic (MHD) model for the interaction between the solar wind and the geomagnetic field, focusing on the approximation of governing equations by classical Chapman-Ferraro theory combined with gas dynamics. The magnetosphere boundary and distant tail are represented by tangential and contact discontinuities, while the bow wave is modeled as a fast MHD shock wave. The connectivity of interplanetary and geomagnetic fields, and the asymptotic directions of the wake and shock waves at great distances from Earth, are analyzed. Numerical results for Mach numbers 5, 8, and 12 for γ = 5/3 and 2 are presented, showing good agreement with observations from shadowgraph photographs of supersonic flow past a model magnetosphere. The distortion of the interplanetary magnetic field in the region between the bow and the magnetosphere is also illustrated for cases with magnetic fields inclined at 45° and 90° to the free-stream direction. The paper explores the application of MHD equations to hypersonic flow of solar plasma around the Earth and its magnetosphere, examines the approximation by gas dynamics, and presents extensive numerical results.The paper discusses a magnetohydrodynamic (MHD) model for the interaction between the solar wind and the geomagnetic field, focusing on the approximation of governing equations by classical Chapman-Ferraro theory combined with gas dynamics. The magnetosphere boundary and distant tail are represented by tangential and contact discontinuities, while the bow wave is modeled as a fast MHD shock wave. The connectivity of interplanetary and geomagnetic fields, and the asymptotic directions of the wake and shock waves at great distances from Earth, are analyzed. Numerical results for Mach numbers 5, 8, and 12 for γ = 5/3 and 2 are presented, showing good agreement with observations from shadowgraph photographs of supersonic flow past a model magnetosphere. The distortion of the interplanetary magnetic field in the region between the bow and the magnetosphere is also illustrated for cases with magnetic fields inclined at 45° and 90° to the free-stream direction. The paper explores the application of MHD equations to hypersonic flow of solar plasma around the Earth and its magnetosphere, examines the approximation by gas dynamics, and presents extensive numerical results.