Rediscussion of eclipsing binaries. XVIII - Faint secondaries in the spectra of early B-type systems

Details Rediscussion of eclipsing binaries. XVIII - Faint secondaries in the spectra of early B-type systems Rediscussion of eclipsing binaries. XVIII - Faint secondaries in the spectra of early B-type systems

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993pasp..105..721p&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 105, no. 689, p. 721-730.

Astronomy and Astrophysics

Astronomy

11

B Stars, Eclipsing Binary Stars, Faint Objects, Stellar Spectra, Charge Coupled Devices, Light Curve, Spectral Line Width, Stellar Evolution, Stellar Luminosity, Stellar Spectrophotometry

Scientific paper

Spectra of three early B-type eclipsing binaries, for which velocities of faint secondary components have been reportedly measured on photographic spectrograms, have been observed with high resolution and signal-to-noise ratio, employing the echelle-CCD Hamilton spectrometer on the 3-m Shane telescope of the Lick Observatory. Very provisional orbits have been rederived for the secondaries in two of the systems, VV Orionis, a main-sequence system, and V380 Cygni, with a highly evolved B0 primary, principally on the basis of velocities from the He I line, 5876 A. Lines in the secondaries of these systems are considerably weaker than previously thought, the 5876 line having equivalent widths of 0.07 and 0.024 A in VV Ori and V380 Cyg, respectively. No line of the secondary was detected unequivocally in the spectrum of the third system, V1765 Cyg, which also has an evolved early B-type primary. The 5876 line is weaker than 0.03 A. An unseen third body causes a variation of the velocity of the center of mass of the close binary in VV Ori, which is poorly determined.

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