Unusual composition of the solar wind in the 2-3 May 1998 CME observed with SWIGS on ACE

Elemental, isotopic and charge state abundances provide valuable information about the source and acceleration mechanism of Coronal Mass Ejections (CMEs). Even though the kinetic properties of the plasma might be subject to changes because of dynamic effects occurring during the expansion of the CME, the composition of the solar wind remains unchanged after it leaves the low corona. Data from the Solar Wind Ion Composition Spectrometer (SWICS) on ACE are used to study the elemental and charge state composition of He, O, C, N, and Fe as well as the isotopic ratio of He during the very large CME of May 2-3, 1998. We find in this CME anomalously large enrichment of He-3(++)/He-4(++), He/O and Fe/O. During the 28 hour long cloud portion of the CME unusually cold material (He-4(+) and very low charge state heavy ions) was observed together with hot (high charge state ions) and normal solar wind plasma.