Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983mnras.204..113a&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 204, July 1983, p. 113-127.
Astronomy and Astrophysics
Astronomy
50
Giant Stars, Hot Stars, Stellar Spectrophotometry, Symbiotic Stars, Variable Stars, Continuous Spectra, Emission Spectra, Infrared Spectra, Radio Spectra, Stellar Envelopes, Stellar Mass Accretion, Ultraviolet Spectra, Visible Spectrum
Scientific paper
The high-excitation emission-line star H1-36 is investigated using optical and infrared spectrophotometry. It is established that H1-36 may be classified as a symbiotic star due to the presence of a variable M giant. The observations are analyzed in terms of the usual binary model for symbiotic stars in which an unseen star is heated by accretion of gas from its companion M giant. It is found that the M giant in H1-36 is very much more highly extinguished than the emission-line region. It is proposed that the circumstellar dust, seen by its thermal emission at infrared wavelengths, surrounds the M giant but not the hotter star, which is the source of photoionization. This indicates that the M giant cannot fill its Roche lobe. The presence of the neutral, circumstellar dust cocoon surrounding the M star is employed to explain the radio spectral shape. It is argued that accretion must be from the M giant's wind if Roche lobe overflow does not occur. The energetics of H1-36 suggest that the accreting component is smaller than a main-sequence star.
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