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.
- Magnetic field structure
- Radial IMF