The spectrum of the VV Cephei star KQ Puppis (Boss 1985). III - A possible model

Details The spectrum of the VV Cephei star KQ Puppis (Boss 1985). III - A possible model The spectrum of the VV Cephei star KQ Puppis (Boss 1985). III - A possible model

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...256..133r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 256, no. 1, p. 133-140.

Astronomy and Astrophysics

Astrophysics

8

Binary Stars, Cepheid Variables, M Stars, Stellar Models, Stellar Spectra, Stellar Spectrophotometry, Balmer Series, Stellar Winds, Ultraviolet Spectra

Scientific paper

KQ Pup is a binary star containing an M supergiant and a hot companion of unclear nature. In the present work, the coude optical spectra of KQ Pup obtained in 1969 at the Dominion Astrophysical Observatory (Canada) and in 1979-1984 at the European Southern Observatory are analyzed. The optical spectrum shows, in addition to the M-star photospheric absorptions, sharp emissions of forbidden S II, Cu II, Fe II, and Ni II, and of Fe II were identified. It is suggested that these emissions arise in an intermediate region of the M-star wind ionized by the hot star radiation. From the blue-IR color indices and the 2200 A interstellar band, a color excess of E(B-V) = 0.14 +/- 0.03 is derived for KQ Pup. The UV to IR energy distribution appears bimodal, with the hot component dominating below about 3600 A and the M Sar above 4000 A.

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