Abstract:
The Helios 1 (H1) and Helios 2 (H2) spacecraft measured the solar winds at a distance between ∼0.3 and 1.0 au
from the Sun. With increasing heliocentric distance (rh), the plasma speed is found to increase at ∼34–40 km s−1
au−1 and the density exhibits a sharper fall (rh-
2) compared to the magnetic field magnitude (r - h
1.5) and the
temperature (rh-
0.8). Using all available solar wind plasma and magnetic field measurements, we identified 68 and
39 fast interplanetary shocks encountered by H1 and H2, respectively. The overwhelming majority (85%) of the
shocks are found to be driven by interplanetary coronal mass ejections (ICMEs). While the two spacecraft
encountered more than 73 solar wind high-speed streams (HSSs), only ∼22% had shocks at the boundaries of
corotating interaction regions (CIRs) formed by the HSSs. All of the ICME shocks were found to be fast forward
(FF) shocks; only four of the CIR shocks were fast reverse shocks. Among all ICME FF shocks (CIR FF shocks),
60% (75%) are quasi-perpendicular with shock normal angles (θBn) 45° relative to the upstream ambient
magnetic field, and 40% (25%) are quasi-parallel (θBn < 45°). No radial dependences were found in FF shock
normal angle and speed. The FF shock Mach number (Mms), magnetic field, and plasma compression ratios are
found to increase with increasing rh at the rates of 0.72, 0.89, and 0.98 au−1, respectively. On average, ICME FF
shocks are found to be considerably faster (∼20%) and stronger (with ∼28% higher Mms) than CIR FF shocks.
