Abstract
We investigate the evolution of solar wind turbulence in the terrestrial foreshock and magnetosheath with a focus on the foreshock region. We analyzed plasma measurements by BMSW instrument on board Spektr-R satellite that has a unique 31 ms time resolution of the ion flux, ion density, solar wind and thermal speeds.
We have found that the spectral power within the fluctuations on all spatial scales increases when we compare the foreshock with solar wind power spectra. In the MHD region, the increase of the foreshock density fluctuations compared to those in the solar wind is more prominent, roughly tenfold, whereas in the kinetic region, the increase is in the order of units.
In the MHD region, the slopes of the power spectra change dramatically, while in the kinetic region, they remain the same.