Analysis and Modeling of the UV Spectra of the Feb. 12, 2000 Flux Rope CME.

Details Analysis and Modeling of the UV Spectra of the Feb. 12, 2000 Flux Rope CME. Analysis and Modeling of the UV Spectra of the Feb. 12, 2000 Flux Rope CME.

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh51b01c&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH51B-01

Physics

7513 Coronal Mass Ejections, 7531 Prominence Eruptions, 7549 Ultraviolet Emissions

Scientific paper

UltraViolet spectra of a typical flux rope CME have been taken with the UltraViolet Coronagraph Spectrometer aboard SOHO above the NW limb at heliocentric distance of 2.3 Rsun. The high temporal and spectral resolutions of the spectra provide a detailed monitoring of the dynamical and physical properties of the CME. Beside the cool lines of H I (1216 and 1025 A) and the intermediate lines of O VI (1032, 1037 A) usually observed in CME this event shows emission in the hot lines of SI XII (520 A) and Mg X (610 A). Doppler shift of the observed spectral lines give the line of sight velocity of the bright front and the prominence core plasma. The latter showing evidence for helical motion. A model of the Doppler shift evolution in both front and core of the CME is presented.

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