Abstract
The solar wind is an ideal environment to enhance our understanding of the collisionless highly-turbulent ionized plasma. It couples two distinct phenomena which are not fully understood, the plasma state of matter and the turbulence.
One open question is the nature of the dissipation mechanism which is responsible for the heating of the solar corona and solar wind. In this study, we analyze a highfrequency part of the power spectra prior to and after the passage of Interplanetary Shocks (IP).
We used the data acquired by BMSW in order to calculate the power spectrum density (PSD) of the ion flux upstream and downstream of the shock. We have found that relative fluctuations in the inertial range are preserved through the shock, whereas the fluctuations in the kinetic range strongly correlate with the gyrostructure frequency.
Our results suggest that the IP shock influences on the nature of the dissipation processes.