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Evolution of the optical spectrum of HM sagittae: 1977--1982

Journal Article · · Astrophys. J.; (United States)
DOI:https://doi.org/10.1086/162043· OSTI ID:6196896

High-resolution spectra have been obtained for HM Sge an V1016 Cygni, two prominent members of the RR Tel family of symbiotic stars. Gaussian fits were made to the emission lines present in those spectra in order to attempt a kinematic separation of the different line-emitting regions expected in those stars. The dominant components of the emission lines for both stars are broad and double-peaked, with peak separations of about 70 km s/sup -1/ and gaussian widths of about 30 km s/sup -1/. Those components are attributed to an expanding, biconical shell created by the interaction of a high-velocity wind from the white dwarf with a preexisting, low velocity wind from the cool star. Narrow, double-peaked components are also present for the forbidden lines of low critical density in HM Sge. Those components presumably originate in the remnant red giant wind external to the shell. The narrow iron lines observed in V1016 Cyg must originate in a high density region, with the best candidate being the atmosphere of the cool star. Evidence for high-velocity gas near the white dwarf, probably in the form of an accretion disk, derives from the great width, FWHM = 490 km s/sup -1/, of the profile for the ''6830'' feature in V1016 Cyg.

Research Organization:
Harvard-Smithsonian Center for Astrophysics
OSTI ID:
6196896
Journal Information:
Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 280:2; ISSN ASJOA
Country of Publication:
United States
Language:
English