Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...288l...5l&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 288, no. 1, p. L5-L8
Astronomy and Astrophysics
Astrophysics
7
Abundance, Asymptotic Giant Branch Stars, Novae, Stellar Envelopes, Stellar Mass Ejection, Symbiotic Stars, Infrared Radiation, Line Spectra, Mass Flow Rate, Oxygen, Radial Velocity, Silicates, Stellar Color, Stellar Luminosity, Ultraviolet Emission
Scientific paper
While a symbiotic nova's outburst quickly degrades the molecular content of a circumstellar shell, it takes approximately 1000 yr to move fresh material out from a star to its OH masing zone. During this post-outburst phase a shell lacks its usual complement of molecules, and so bears a stamp from the nova outburst, even though it is no longer a soft X-ray, UV or radio source. These objects are 'fossil' symbiotic novae. The number of potential 'fossils' with dense shells is commensurate with the frequency of observed Galactic symbiotic novae. The densest O-rich shells exhibit the 9.7 micrometers silicate line in absorption. This places them in the IRAS low resolution spectral type 38-39 class. About 50% of these mass-losing giants have had comparably massive companions. Of 38 class members examined at 1612 MHz, 32 exhibit masers. But six (16%) lack them. We identify these six with 'fossil' symbiotic novae.
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