Authors: P. Wurz, F.M. Ipavich, A.B. Galvin, P. Bochsler, M.R. Aellig, R. Kallenbach, D. Hovestadt, H. Grünwaldt, M. Hilchenbach, W.I. Axford, H. Balsiger, A. Bürgi, M.A. Coplan, J. Geiss, F. Gliem, G. Gloeckler, S. Hefti, K.C. Hsieh, B. Klecker, M.A. Lee, S. Livi, G.G. Managadze, E. Marsch, E. Möbius, M. Neugebauer, K.U. Reiche, M. Scholer, M.I. Verigin, and B. Wilken
Reference: Geophys. Res. Lett. 25(14) (1998) 2557-2560.
Using solar wind particle data from the CELIAS/MTOF sensor on the SOHO mission, we studied the abundance of the elements O, Ne, Mg, Si, S, Ca, and Fe for the time period around the January 6, 1997, coronal mass ejection event (CME). In the interstream and coronal hole regions before and after this event we found elemental abundances consistent with the expected abundance patterns of the respective flow regimes. However, during the passage of the CME and during the passage of the erupted filament, which followed the CME, we found that the elemental composition differed markedly from the interstream and coronal hole regions before and after this event. During the passage of the CME and the passage of the erupted filament we found a mass-dependent element fractionation, with a monotonic increase toward heavier elements. We observed Si/O and Fe/O abundance ratios of about one half during these time periods, which is significantly higher than for typical solar wind.