Spectroscopic observations of PU Vulpeculae and its binary nature

Details Spectroscopic observations of PU Vulpeculae and its binary nature Spectroscopic observations of PU Vulpeculae and its binary nature

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986acaps...6..193l&link_type=abstract

(Acta Astrophysica Sinica, vol. 6, 1986, p. 193-199) Chinese Astronomy and Astrophysics (ISSN 0275-1062), vol. 10, Dec. 1986, p.

Astronomy and Astrophysics

Astrophysics

1

Binary Stars, Novae, Peculiar Stars, Stellar Spectrophotometry, Absorption Spectra, Abundance, Balmer Series, Emission Spectra, F Stars, H Alpha Line, M Stars

Scientific paper

The peculiar nova-like star PU Vul was observed spectroscopically from Sept. 12, 1981 to Dec. 11, 1983 at Yunnan Observatory and Beijing Observatory. In Sept. 1981, the star showed an absorption spectrum of the Balmer lines, the H, K, and D lines, and some Fe II, Sr II, and Ti II lines. H-alpha was seen in emission in Oct. 1982 and H-beta, in Sept. 1983. Both emissions were enhanced in Oct. 1983, and then dimmend since Nov. 1983. On Dec. 11, 1983 H-beta might be absent, but the H-alpha was still visible. The spectral type was similar to that of an F giant during this period. This object may be an exceptionally slow nova and a binary consisting of an M giant and a hot companion.

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