Temporal profiles of solar wind parameters from 3 to 9 August 2017 (215–221 doy), at a time resolution of 6 s. Panels show from top to bottom the proton velocity components in the HEE reference system, V_x (panel a), V_y (panel b), and V_z (panel c), the proton number density (panel d) and proton temperature (panel e), the magnetic field magnitude (panel f) and the magnetic field components in HEE, B_x (panel g), B_y (panel h), and B_z (panel i), and the angle θ = cos⁻¹(|B_x|/|B|) between the average magnetic field direction and the radial direction (panel j). In the last panel, the dashed black curve represents the local Parker spiral direction, with respect to the high-speed region and rarefaction region. The dashed red line in each panel denotes the velocity knee between the fast-wind region and the rarefaction region. At the top of the figure we indicate the different solar wind regions vertically. The colors correspond to the sketch in Fig. 1.