A comparison of the IMF structure and the magnetic field in the magnetosheath under the radial IMF conditions

In previous studies, the magnetic field structures in the solar wind and in the magnetosheath usually have a high dependence on only the Y component. In this study, we compared the simultaneous data from OMNI database, THEMIS-B in the solar wind, and THEMIS-C in the magnetosheath to investigate the relationship between the magnetic field structures in the solar wind and in the magnetosheath under the radial IMF conditions. We find that B _z has a better correlation than B _y between the magnetic fields in the two regions, and the correlation for B _x is poor. When the magnetic field transits through the bow shock, the magnetic field will be enhanced in all components, especially in B _y . After that, B _x will divert to the Y and Z components, but the diversion to B _y will be larger than that to B _z in this case.