Ultraviolet Coronagraph Spectrometer Observation of the 1996 December 23 Coronal Mass Ejection

Details Ultraviolet Coronagraph Spectrometer Observation of the 1996 December 23 Coronal Mass Ejection Ultraviolet Coronagraph Spectrometer Observation of the 1996 December 23 Coronal Mass Ejection

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...491l..59c&link_type=abstract

Astrophysical Journal Letters v.491, p.L59

Astronomy and Astrophysics

Astronomy

23

Sun: Corona, Sun: Uv Radiation, Sun: Prominences

Scientific paper

The Ultraviolet Coronagraph Spectrometer (UVCS) aboard the Solar and Heliospheric Observatory (SOHO) observed a spectacular coronal mass ejection (CME) caused by a prominence eruption on 1996 December 23. The evolution of the ejected prominence material was followed for 1 hr and 50 minutes. The observation consists of a series of 5 minute exposures, at a fixed heliocentric distance of 1.5 R solar in several spectral ranges. The Lyman lines of hydrogen brighten more than 2 orders of magnitude during the CME. The C III 977.02 A line is very bright, and many other low-temperature lines have been detected. Line intensities and profiles provide important diagnostics for the physical and dynamical parameters of the ejected plasma. Lines widths show nonthermal line broadening due to a plasma expansion with velocity larger than 50 km s-1. The Ly alpha inside the CME region shows red and blue shifts, up to 0.2 A (50 km s-1) and 0.8 A (200 km s-1), respectively. A preliminary estimate shows a flat emission measure distribution 3 or 4 orders of magnitude smaller than typical prominence emission measures. Essentially the same structure in space and velocity is seen in the Lyman lines, in C III ( 105 K) and in O VI ( 3x105 K).

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