Steady-state magnetic field in the magnetosheath

A numerical method is presented for finding the magnetic field in the transition region between the bow shock and the effective obstacle in steady state three dimensional solar wind flow around a planet. On assuming that the Alfven-Maeh number is very large there is decoupling into a gasdynamic problem and an electromagnetic problem. After solving the gasdynamic problem in the axisymmetric formulation, the equations for the magnetic field are also solved numerically. A comparison with earlier solutions is made. The results are discussed from the point of view of their possible use in the interpretation of satellite data.