HR: 0800h
AN: SH21B-0402    [Abstracts]
TI: A Detection of the Same Hot Plasma in the Corona - During a CME - and Later at Ulysses
AU: * Suess, S T
EM: Steven.T.Suess@nasa.gov
AF: NASA Marshall Space Flight Center, Natl. Space Science & Technology Ctr., Mail Stop SD50, Huntsville, AL 35812 United States
AU: Poletto, G
EM: poletto@arcetri.astro.it
AF: Arcetri Astrophysical Observatory, (Instituto Nazionale di Astrofisica), Largo Enrico Fermi, 5, Florence, 50125 Italy
AU: Bemporad, A
EM: bempy76@arcetri.astro.it
AF: Dipartimento di Astronomia e Scienza dello Spazio, University of Florence, Largo Enrico Fermi, 2, Florence, 50125 Italy
AB: We show direct evidence for the same very hot plasma being detected remotely from SOHO in the corona and subsequently, {\it in situ}, at Ulysses in the solar wind. This is, to our knowledge, the first time that such an unambiguous identification has been made in the case of hot plasma. This detection complements studies correlating other plasma and field properties observed {\it in situ} to the properties measured at the source in the corona. This observation takes advantage of a SOHO-Sun-Ulysses quadrature, during which the Sun-Ulysses included angle is $90^\circ$ and it is possible to observe {\it in situ} with Ulysses instruments the same plasma that has previously been remotely observed with SOHO instruments in the corona on the limb of the Sun. The identification builds on an existing base of separate SOHO and interplanetary detections of hot plasma. SOHO/UVCS has found evidence for very hot coronal plasma in current sheets in the aftermath of CMEs (Ciaravella et al., 2002; Raymond et al., 2003; Ko et al., 2002) in the [Fe XVIII] $\lambda$ 974 \AA\ line, implying a temperature on the order of $6 \times 10^6$ K. This temperature is unusually high even for active regions, but is compatible with the high temperature predicted in current sheets. In the solar wind, ACE data from early 1998 to middle 2000 revealed high frozen-in Fe charge state (Fe$^{16+}$)in many cases to be present in interplanetary plasma (Lepri et al., 2004). These identifications were associated with ICMEs. Ciaravella, A., Raymond, J. C., Li, J., Reiser, P., Gardner, L. D., Ko, Y.-K., & Fineschi, S. 2002, Astrophys. J., 575, 1116 Ko, Y.-K., Raymond, J. C., Li, J., Ciaravella, A., Michels, J., Fineschi, S., & Wu, R. 2002, Astrophys. J., 578, 979 Lepri, S. T., & Zurbuchen, T. H. 2004, J. Geophys. Res., 109(A1), A01112 Raymond, J. C., Ciaravella, A., Dobrzycka, D., Strachan, L., Ko, Y.-K., & Uzzo, M. 2003, Astrophys. J., 597, 1106
DE: 7513 Coronal mass ejections
DE: 2111 Ejecta, driver gases, and magnetic clouds
DE: 2169 Sources of the solar wind
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting