ИСТИНА

The solar wind magnetic clouds are manifestations of solar activity causing the most noticeable geomagnetic disturbances. This is due to the fact that they are distinguished by the presence of regions with a strong regular IMF and sharp fronts. Studies have shown that in many cases the body of a magnetic cloud is preceded by a shock wave on the leading edge of the cloud. In this case, a turbulent sheath between the shock wave and the leading edge of the magnetic cloud is detected. So it is interest to study the relationship between geomagnetic activity and the magnetic cloud structure. The proposed study establishes the dependence of the high-latitude geomagnetic activity level on the intensity of turbulent processes occurring at the leading edge of the magnetic field. In turn, turbulent phenomena in magnetic cloud sheath are largely determined by the orientation of the wave shock plane with respect to the IMF absorbed by the shock wave as it propagates in the solar wind. It is common to distinguish between the terms of a quasi-parallel and quasi-perpendicular shock wave associated with the level of sheath turbulence following the shock wave. Therefore, the proposed metho d of searching for shock waves in the solar wind flux from the spacecraft data is a necessary part of the investigation. The detection and calculation of their shock planes orientation allow us to conclude that the turbulent sheath is also disturbed. In its turn, the disturbance degree of magnetic clouds sheath with the intensity level of the substorm processes is correlated.