Quiescent prominence spectrophotometry - Sodium D1,2, helium D3, and calcium /plus/ lambda 8498

Details Quiescent prominence spectrophotometry - Sodium D1,2, helium D3, and calcium /plus/ lambda 8498 Quiescent prominence spectrophotometry - Sodium D1,2, helium D3, and calcium /plus/ lambda 8498

Dec 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...251..768l&link_type=abstract

Astrophysical Journal, Part 1, vol. 251, Dec. 15, 1981, p. 768-780.

Astronomy and Astrophysics

Astrophysics

13

Calcium, Helium, Line Spectra, Sodium, Solar Prominences, Stellar Spectrophotometry, Coronagraphs, Emission Spectra, Radiant Flux Density, Solar Spectra, Solar Temperature, Stellar Models, Stellar Structure, Velocity Distribution, Vertical Distribution, Vidicons

Scientific paper

The reported observations were carried out by means of a 25 cm coronagraph/coude spectrograph with a Si vidicon Optical Multichannel Analyzer (OMA) detector. The results of the investigation are presented in a number of tables, and the main conclusions concerning the studies are discussed. The relative behavior of prominence Na D line emission shows that the employed observing techniques yield reliable measures of prominence line strengths, not degraded to any substantial extent, in particular, by possible slit-filling effects. This conclusion is limited principally by the assumption that systematic vertical velocity fields in the prominences are not greater than 1.5 km/s. The Na D line profiles are well fitted by a one-component (i.e., homogeneous) line-forming region, thus reinforcing previous conclusions regarding the source of the enhanced wing emission.

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