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We investigated a set of 54 interplanetary coronal mass ejection (ICME)events whose solar sources are very close to the disk center (within 15 degreesfrom the central meridian). The ICMEs consisted of 23 magnetic cloud (MC)events and 31 non-MC events. Our analyses suggest that the MC and non-MC ICMEshave more or less the same eruption characteristics at the Sun in terms of softX-ray flares and CMEs. Both types have significant enhancements in chargestates, although the non-MC structures have slightly lower levels ofenhancement. The overall duration of charge state enhancement is alsoconsiderably smaller than that than that in MCs as derived from solar windplasma and magnetic signatures. We find very good correlation between the Feand O charge state measurements and the flare properties such as soft X-rayflare intensity and flare temperature for both MCs and non-MCs. Theseobservations suggest that both MC and non-MC ICMEs are likely to have aflux-rope structure and the unfavorable observational geometry may beresponsible for the appearance of non-MC structures at 1 AU. We do not find anyevidence for active region expansion resulting in ICMEs lacking a flux ropestructure because the mechanism of producing high charge states and the fluxrope structure at the Sun is the same for MC and non-MC events.

The Solar Connection of Enhanced Heavy Ion Charge States in the Interplanetary Medium: Implications for the Flux-rope Structure of CMEs