Spectroscopic observations of eclipsing binaries. V - Accurate mass determination for the B-type systems V539 Arae and Zeta Phoenicis

Details Spectroscopic observations of eclipsing binaries. V - Accurate mass determination for the B-type systems V539 Arae and Zeta Phoenicis Spectroscopic observations of eclipsing binaries. V - Accurate mass determination for the B-type systems V539 Arae and Zeta Phoenicis

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...118..255a&link_type=abstract

Astronomy and Astrophysics, vol. 118, no. 2, Feb. 1983, p. 255-261. Statens Naturvidenskabelige Forskningsrad

Astronomy and Astrophysics

Astrophysics

31

B Stars, Eclipsing Binary Stars, Stellar Mass, Stellar Spectra, Angular Velocity, Companion Stars, Line Spectra, Orbital Elements

Scientific paper

Radial velocities from new 12 Å/mm coudé spectra yield much improved spectroscopic orbits and mass determinations for the two B-type double-lined eclipsing binaries V539 Ara (B3V + B4V) and ζ Phe (B6V + B8V). Combining these orbits with published photometric analyses, absolute dimensions of excellent accuracy (1-2 %) are derived for the components (Table 7). These agree well with the theoretical stellar models by Hejlesen (1980).
Earlier reported distortions of the velocity curves of the Balmer lines in V539 Ara, interpreted as due to gas streams, are found to be due merely to line blending, and no mass transfer seems to take place. A more definitive photometric study of this system is needed. The measured rotational velocities agree well with those expected for synchronous rotation for both primary components, but indicate that the secondary of V539 Ara rotates somewhat slower, and the secondary of ζ Phe appreciably faster, than synchronism. Apsidal motion is detected in both systems.
In the new spectrograms of ζ Phe, spectral lines of the close (0".5), physically bound A-type visual companion could also be measured. The somewhat discrepant radial velocities of the two more distant companions to both systems make their physical connection with the eclipsing pairs doubtful.

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