AAS 200th meeting, Albuquerque, NM, June 2002
Session 37. CMEs and Prominences
Display, Tuesday, June 4, 2002, 10:00am-6:30pm, SW Exhibit Hall

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[37.18] Transverse Prominence Motions from 10,000-250,000 K

T.A. Kucera (NASA/GSFC), M. Tovar (California State Northridge), B. De Pontieu (Lockheed-Martin)

We address the origin of prominence material by comparing high cadence (30-60 s) He I and O V EUV observations from SOHO/CDS wide slit movies, and also, for another prominence observation, observations from TRACE at 1216 Å\ and 1600 Å\ and SVST in H\alpha. The EUV and UV observations regularly show small scale structures with plane-of-the-sky velocities of 20-80 km/s. Many, although not all, of these motions are seen in multiple wavelength bands, representing temperatures ranging from 10,000 -- 100,000 K or 20,000 -- 250,000 K, depending on the data set. The H\alpha observations contain line shift information showing clearly that the associated UV prominence intensity motions do actually represent real mass motions, as opposed to temperature or density waves. The results indicate that the ``prominence-corona transition region'' is not an outside layer to the prominence as a whole, but is rather associated with smaller scale structures all through the prominence.

Support for this work was provided by NASA SR&T Grant NASW-00034. SOHO is a joint project of ESA and NASA.

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Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.