The C IV doublet ratio intensity effect in symbiotic stars

Details The C IV doublet ratio intensity effect in symbiotic stars The C IV doublet ratio intensity effect in symbiotic stars

Aug 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...331..477m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 331, Aug. 1, 1988, p. 477-485.

Other

21

Carbon, Fine Structure, Spectrum Analysis, Stellar Spectra, Symbiotic Stars, H Ii Regions, High Resolution, Omicron Ceti Star, Spectral Resolution, Stellar Winds, Ultraviolet Spectra

Scientific paper

High-resolution UV spectra in the 1200-2000 wavelength range of the symbiotic variable R Aqr and its nebular jet were obtained in July 1987 with the IUE. The line profile structure of the C IV 1548, 1550 doublet in the jet indicates multicomponent velocity structure from an optically thin emitting gas. The C IV doublet profiles in the compact H II region engulfing the Mira and hot companion binary also suggest multicomponent structure with radial velocities up to about -100 km/s. The value of the doublet intensity ratio in the R Aqr H II region has been observed in other similar symbiotic stars, such as RX Pup. It is suggested that the anomalous behavior of the C IV doublet intensities may be useful for studying the spatial structure and temporal nature of winds in symbiotic stars.

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