Identification of the emission bands at 6830, 7088 A

Details Identification of the emission bands at 6830, 7088 A Identification of the emission bands at 6830, 7088 A

Mar 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...211l..31s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 211, no. 2, March 1989, p. L31-L34. Research supported by SNSF.

Astronomy and Astrophysics

Astrophysics

134

Binary Stars, Emission Spectra, Line Spectra, Oxygen Spectra, Stellar Spectra, Symbiotic Stars, Giant Stars, Hot Stars, Hydrogen, Raman Spectra, Scattering Cross Sections, Spectrum Analysis

Scientific paper

Broad emission bands at 6830 and 7088 A are observed in more than 50 percent of symbiotic stars. Up to now these features have not been identified. They have only been observed in spectra of symbiotic binaries, which show high excitation emission and M-type absorption. It is suggested that the emission features are due to Raman scattering of the OVI resonance doublet 1032, 1038 A by neutral hydrogen. In this process the OVI photons are absorbed by hydrogen in its ground state 1s2S.

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