Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...280..695s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 280, May 15, 1984, p. 695-711.
Astronomy and Astrophysics
Astrophysics
31
Companion Stars, High Resolution, Red Giant Stars, Stellar Spectra, Visible Spectrum, White Dwarf Stars, Astronomical Catalogs, Emission Spectra, Line Spectra, Radiant Flux Density, Spectral Line Width, Stellar Envelopes, Stellar Evolution, Stellar Models, Stellar Winds
Scientific paper
High-resolution spectra have been obtained for HM Sge and 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 kinemaic separation of the different line-emitting regions expected in those stars. The dominant emission lines 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. Twenty eight low-resolution spectra of HM Sge were obtained during the period 1977 June through 1982 June. Relative fluxes for emission lines in the 3800 - 8300 Å region have been derived from those spectra. Prior to 1979 August, the effective temperature of the hot star was less than 70,000K. By 1980 May, the temperature of the hot star had increased to 160,000K. A plausible model for the system is that the 1975 outburst of HM Sge resulted from a hydrogen flash in the accretion envelope of the white dwarf. The 1979 transition occurred when the wind from the white dwarf completed removal of that envelope, exposing the hotter core of the white dwarf.
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