IUE and optical spectral scans of U Sagittae - an analysis and comparison with U Cephei

Details IUE and optical spectral scans of U Sagittae - an analysis and comparison with U Cephei IUE and optical spectral scans of U Sagittae - an analysis and comparison with U Cephei

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985pasp...97..138d&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 97, Feb. 1985, p. 138-150.

Astronomy and Astrophysics

Astronomy

22

Cepheid Variables, Eclipsing Binary Stars, Stellar Composition, Stellar Spectra, Ultraviolet Astronomy, Visible Spectrum, Abundance, Iue, Photosphere, Radial Velocity, Stellar Rotation

Scientific paper

Recent optical and ultraviolet observations of U Sge are presented, and the results are compared with observations of U Cephei. The observations were carried out with: the International Ultraviolet Explorer (IUE) satellite; with the ITS scanner of the Lick Observatory; and with a Varo image-tube camera attached to a coude spectrograph. Comparison with data for U Ceph showed that U Sge is of the B7.5 V spectral type with an effective temperature of 12,250 + or 250 K, and a surface gravity of 3.9 + or - 0.1 log g. The secondary component of U Sge appears to be of the G4 III-IV spectral type. The best estimate for the distance of U Sge was 295 + or - 20 pc. Emission lines of the W Serpentis type were found in the IUE spectrum for U Sge. Although the observed fluxes for the lines were low, the powers were half as strong as those observed in U Cep. Selected emission lines of Fe II, Si II, and Si III were also found assuming solar abundances. A complete summary of the IUE and optical data is provided in a series of graphs and tables.

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