Tomographic separation of composite spectra. I - The components of Plaskett's Star

Details Tomographic separation of composite spectra. I - The components of Plaskett's Star Tomographic separation of composite spectra. I - The components of Plaskett's Star

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...385..708b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 385, Feb. 1, 1992, p. 708-717. Previously announced in STAR as N91-28050.

Astronomy and Astrophysics

Astrophysics

38

Algorithms, Binary Stars, Computer Aided Tomography, Line Spectra, O Stars, Stellar Spectra, Ultraviolet Spectra, Angular Resolution, Hertzsprung-Russell Diagram, Mass Ratios, Photosphere, Spectrum Analysis, Stellar Evolution, Stellar Mass, Stellar Winds

Scientific paper

The UV photospheric lines of Plaskett's Star (HD 47129), a 14.4 day period, double lined O-type spectroscopic binary were analyzed. Archival data from IUE (17 spectra well distributed in orbital phase) were analyzed with several techniques. A cross correlation analysis, which showed that the secondary produces significant lines in the UV, indicates that the mass ratio is q = 1.18 +/- 0.12 (secondary slightly more massive). A tomography algorithm was used to produce the separate spectra of the two stars in six spectral regions. The interpolated spectral classifications of the primary and secondary, 07.3 I and 06.2 I, respectively, were estimated through a comparison of UV line ratios with those in spectral standard stars. The intensity ratio of the stars in the UV is 0.53 +/- 0.05 (primary brighter). The secondary lines appear rotationally broadened, and the projected rotational velocity V sin i for this star is estimated to be 310 +/- 20 km/s. The possible evolutionary history of this system is discussed through a comparison of the positions of the components and evolutionary tracks in the H-R diagram.

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