Generally, in situ parameters of interplanetary coronal mass ejections (ICMEs) are analyzed as a whole, or ICMEs are classified by speed or whether they are with and without magnetic clouds. Zhai and colleagues found that ICMEs with and without flares can be extracted only by the average charge states of iron (Q Fe). In the present study, the ICMEs are categorized into two types, flare CMEs (FCs) and nonflare CMEs (NFCs) by the Q Fe. We find that the occurrence rates of FCs and NFCs are both decreased from solar maximum to minimum. The occurrence rates and proportions of FCs are both higher in solar cycle 23 than in solar cycle 24. In contrast, the occurrence rates of NFCs are almost the same during the two solar cycles. The durations of FCs are longer than those of NFCs. The fractions of FCs and NFCs that are associated with magnetic clouds (MCs) or magnetic field direction rotation evidence are 73% and 69%, respectively. The speed, Q Fe, O7+/O6+, helium abundance (A He), and first ionization potential bias are all higher for FCs than for NFCs. The above parameters inside NFCs and solar wind are almost the same. The solar cycle dependence of the parameters inside NFCs is more clear than that inside FCs. The statistical results demonstrate that the material sources of FCs are not completely the same as those of NFCs. Part of the material inside FCs should come from the lower atmosphere where the A He is higher. The statistical results indicate that all CMEs are associated with flux ropes on the Sun.

The properties of active regions and their connections with the solar wind are important issues. In this study, nine isolated active regions near the solar disk center were chosen. The relationships between blueshift, intensity, magnetic concentrated areas (MCAs), and the potential-field source-surface (PFSS) open magnetic field of active regions were analyzed. Whether an active region contributes to the solar wind was identified only based on the relationship between the properties of in situ solar wind and the large structure of the corona. Then the two phenomena (blueshift and PFSS open magnetic field) for inferring whether an active region contributes to the solar wind were tested. We find that the blueshift areas appear in all cases and the average Doppler speed ranges from −6 to −23 km s−1. The blueshift areas generally root inside MCAs and are far from the neutral lines. The intensity of blueshift areas negatively correlates with the blueshift speed. Statistically, 10 of 16 blueshift areas are associated with the PFSS open magnetic field lines, and all 10 PFSS open magnetic field areas are accompanied by blueshift. We demonstrate that a polarity of an active region generally contributes to the solar wind if it is associated with a PFSS open magnetic field. There are 9 of 10 (13 of 16) PFSS open magnetic field areas (blueshift regions) associated with the solar wind. The results of this study should help determine the observation target of SPICE on board the Solar Orbiter whose scientific goal is connecting the Sun and the heliosphere.