O VI /lambda equals 1032 A/ profiles in and above an active region prominence, compared to quiet sun center and limb profiles

Details O VI /lambda equals 1032 A/ profiles in and above an active region prominence, compared to quiet sun center and limb profiles O VI /lambda equals 1032 A/ profiles in and above an active region prominence, compared to quiet sun center and limb profiles

Nov 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980soph...68..187v&link_type=abstract

Solar Physics, vol. 68, Nov. 1980, p. 187-206. Centre National d'Etudes Spatiales

Physics

20

Line Shape, Oxygen Spectra, Solar Limb, Solar Prominences, Spectroheliographs, Chromosphere, Data Reduction, Oso-8, Satellite Observation, Solar Corona, Solar Physics, Spectral Line Width

Scientific paper

O VI (λ = 1032 Å) profiles have been measured in and above a filament at the limb, previously analyzed in H I, Mg II, Ca II resonance lines (Vial et al., 1979). They are compared to profiles measured at the quiet Sun center and at the quiet Sun limb.
Absolute intensities are found to be about 1.55 times larger than above the quiet limb at the same height (3"); at the top of the prominence (15" above the limb) one finds a maximum blue shift and a minimum line width. The inferred non-thermal velocity (29 km s-1) is about the same as in cooler lines while the approaching line-of-sight velocity (8 km s-1) is lower than in Ca II lines.
The O VI profile recorded 30" above the limb outside the filament is wider (FWHM 0.33 Å). It can be interpreted as a coronal emission of 0 VI ions with a temperature of about 106 K, and a non-thermal velocity (NTV) of 49 km s-1. This NTV is twice the NTV of quiet Sun center O VI profiles. Lower NTV require higher temperatures and densities (as suggested by K-coronameter measurements). Computed emission measures for this high temperature regime agree with determinations from disk intensities of EUV lines.

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