Liudmila Rakhmanova ^* Alexander Khokhlachev Maria Riazantseva Yuri Yermolaev Georgy Zastenker

• Space Research Institute (RAS), Moscow, Russia

Turbulent solar wind is known to be a main driver of the processes inside the magnetosphere including geomagnetic storms and substorms. Experimental studies of the last decade demonstrate additional ways of interplanetary plasma transport to the magnetosphere including small-scale processes in the magnetosphere boundary layers. This fact implies that properties of the solar wind turbulence can affect the geomagnetic activity. However, in front of the magnetosphere there are a bow shock and a magnetosheath region which contribute to the changes of the properties of the solar wind turbulence and may result in destructions of the link between the solar wind turbulence and the magnetosphere. Present study provides the statistics of two-point simultaneous measurements of the turbulence properties in the solar wind and in the magnetosheath based on Wind and THEMIS spacecraft data. Changes in the turbulence properties are analyzed for different background conditions. Solar wind bulk speed and temperature are shown to be the main factors which influence the modification of turbulence at the quasi-perpendicular bow shock at the frequencies higher than the break frequency (ion transition range). Inside the magnetosheath, significant steepening of spectra occurs with increase of temperature anisotropy without connection to the upstream spectra scaling that underlines crucial role of the instabilities in turbulence properties behind the bow shock.