High Velocity and Rapidly Variable Emission Features in the Spectra of Rs-Ophiuchi and Ch-Cygni

Details High Velocity and Rapidly Variable Emission Features in the Spectra of Rs-Ophiuchi and Ch-Cygni High Velocity and Rapidly Variable Emission Features in the Spectra of Rs-Ophiuchi and Ch-Cygni

Mar 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...283..919i&link_type=abstract

Astronomy and Astrophysics, Vol. 283, NO. 3/MAR(III), P. 919, 1994

Astronomy and Astrophysics

Astrophysics

19

Stars Individual: Rs Oph, Ch Cyg - Stars: Symbiotic - Outflows

Scientific paper

Spectroscopic observations in the optical region of the recurrent nova, and symbiotic star, RS Oph were carried out during the years from 1988 to 1992. This object was in a quiescent stage after the outburst in 1985. We found, however, that its spectral features were not quiescent. In most spectra the emission lines of H I, and probably also of He I, were accompanied by broad emission components whose wavelength, profile, and intensity were strongly variable with a time scale of days. The broad components appeared either in the blue or in the red side of the narrow lines, but usually not in both sides simultaneously. During our observations the broad components were found to lie more frequently in the blue side than in the red side. The broad components have shown a double peak profile in most spectra, and more complicated profiles were also observed. Sometimes even in the same spectrum, broad components of different Balmer lines were observed with different profiles. The displacements of the center of the double peak with respect to the narrow lines were found in a range from -1300 km s-1 to +1050 km s-1, but most of them were concentrated in four discrete ranges of-1220‰25km s-1 and -1140±15 km s-1 in the blue side,and +1020±25km s-1 and +930‰20 km s-1 in the red side. The width of the gap of the double peak was varying in a range from 200 km s-1 to 800 km s-1, and when one peak had a larger displacement, the other was less displaced.
No trace of similar emission features was found in spectra of many symbiotic stars in our archives (e.g. Z And, AX Per, AG Dra, HM Sge, BF Cyg, CI Cyg, V1016 Cyg, V1329 Cyg). In some recent spectra of CH Cyg, however, variable broad emission components of H I lines are noticed.

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