tokens: processes. Interestingly, the relation between av Q C and av Q O of the ICME materials is different from that of the carbon-cold materials inside the ICMEs reported by Feng et al. ( 2018 ). The carbon-cold materials are defined by the carbon ionic charge state, which should be relatively lower than the solar wind mean value by three times standard deviation, with the ionic temperature lower than 10 6.05 K. It supports the distinct source or heating process of prominence materials and coronal materials in ICMEs. Further, there are three types of charge distributions inside the studied ICMEs excluding the cold material. Similar results are reported by Rivera et al. ( 2019 ) from their case study, who identified and studied the different types from the different sources in depth. Our statistical results support the stable existence of the different types of charge distributions of heavy ions during most years of a solar cycle. And the fractions of these charge distributions show clear dependence on the solar cycle. This means that the combination of the materials from different sources is common in ICMEs, but the fraction of them would change according to the solar activity. It also implies that the acceleration, the heating process, and the freeze-in height in CMEs may be different between the solar maximum and solar minimum. The source of heavy ions and the heating processes are possibly under modulation by the status of the solar magnetic field. As the most abundant heavy ions in the solar atmosphere (Asplund et al. 2009 ), oxygen ion flux in the solar wind has been systematically studied by von Steiger et al. ( 2010 ). It distributes from 10 4 to 10 6 cm −2 s −1 in the slow solar wind, and from 10 4.5 to 10 5.5 cm −2 s −1 in the fast solar wind. The peaks of the two distributions are a bit less and a bit more than 10 5 cm −2 s −1 , respectively. In the 281 ICMEs, the oxygen flux varies from 2 × 10 4 to 1.5 × 10 5 cm −2 s −1 . And it fluctuates around 10 5 cm −2 s −1 during the solar maximum, when the annual mean SN is more than 60. It could be identified that the oxygen flux in ICMEs is similar to that in the solar wind. Since the SN represents the status of the solar magnetic field, the quasi-linear relation between the O flux in the ICMEs and the SN, when the SN is less than 60, indicates that the O flux is possibly related to the status of the solar magnetic field. 5. Conclusion This statistical work analyzes the abundances and the charge states of heavy ions in the 281 ICMEs from 1998 to 2011. The mean proton speed of the ICMEs and the average charge states of heavy ions are highly related to the solar cycle. Since the SN represents the state of the solar magnetic field by nature, the proton speed and heavy ion composition of ICMEs are possibly related to the solar magnetic field. Another interesting result is the classification effect of the speed on the abundances and charge states of heavy ions. Similar to the solar wind, ICMEs could
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