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Magnetic clouds (MCs) are the interplanetary counterpart of coronal magneticflux ropes. They can provide valuable information to reveal the flux ropecharacteristics at their eruption stage in the corona, which are unable to beexplored in situ at present. In this paper, we make a comprehensive survey ofthe average iron charge state (<Q>Fe) distributions inside 96 MCs for solarcycle 23 using ACE (Advanced Composition Explorer) data. As the <Q>Fe in thesolar wind are typically around 9+ to 11+, the Fe charge state is defined ashigh when the <Q>Fe is larger than 12+, which implies the existence of aconsiderable amount of Fe ions with high charge states (e.g., \geq 16+). Thestatistical results show that the <Q>Fe distributions of 92 (~ 96%) MCs can beclassified into four groups with different characteristics. In group A (11MCs), the <Q>Fe shows a bimodal distribution with both peaks higher than 12+.Group B (4 MCs) presents a unimodal distribution of <Q>Fe with its peak higherthan 12+. In groups C (29 MCs) and D (48 MCs), the <Q>Fe remains higher andlower than 12+ throughout ACE passage through the MC, respectively. Possibleexplanations to these distributions are discussed.

A Statistical Study of the Average Iron Charge Distributions inside Magnetic Clouds for Solar Cycle 23