to the 26-kK value observed by Chien. The second transition \ps -* (core) (b2)1 (ai)2(a2)1 (ai)1 gives 36.5 compared to the 37 kK measured. We know however that the a2 and a2 levels should be reversed, which involves the 7 kK which separates them.We conclude that the "crystal field terms" play a significant role in a valid discussion of the electronic structure of (CóHs)2VC12. Though the type II calcula-D. W. Clack and J. R. Yandle tion predicts a ground state of incorrect symmetry, our previous discussion indicates that an energy shift of about 7 kK produces a MO picture which is in reasonable agreement with both the optical and epr data.Acknowledgments.-We acknowledge gratefully the partial support of this work by the National Science Foundation under Grant GP-10063.

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We describe Wind observations of two lunar wake encounters which occurred on 12–13 November 1996 and 18 July 2002. The observations were made at downstream distances of around 25 and 15 lunar radii (RL), respectively. Both encounters occurred prior to the spacecraft entering the lunar shadow; one event took place within the magnetosheath. A characteristic feature of the lunar wake is the presence of two counterstreaming ion beams drawn in from either flank. We find that both ion components exhibit an extreme temperature anisotropy, often with T⊥ ∼ 10T∥. The anisotropy is greatest in the central wake region. It appears that the anisotropy arises through the conservation of adiabatic invariants as solar wind plasma expands to fill in the cavity behind the Moon. Despite their large anisotropy, the proton distributions appear stable to the cyclotron instability. Correlated field and flow directional changes show that the wake geometry is dependent upon the prevailing magnetic field orientation.

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