ICCD speckle observations of binary stars. XIX - an astrometric/spectroscopic survey of O stars

Details ICCD speckle observations of binary stars. XIX - an astrometric/spectroscopic survey of O stars ICCD speckle observations of binary stars. XIX - an astrometric/spectroscopic survey of O stars

Feb 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aj....115..821m&link_type=abstract

Astronomical Journal, vol. 115, p. 821

Astronomy and Astrophysics

Astronomy

240

Binary Stars, Astrometry, Stellar Spectrophotometry, O Stars, Speckle Interferometry, Open Clusters, Radial Velocity, Mass Distribution

Scientific paper

We present the results of a speckle interferometric survey made with the CHARA speckle camera and 4 m class telescopes of Galactic O-type stars with V less than 8. We can detect with the speckle camera binaries in the angular separation range 0.035-1.5 arcsec with delta M less than 3, and we have discovered 15 binaries among 227 O-type systems. We combined our results on visual binaries with measurements of wider pairs from the Washington Double Star Catalog and fainter pairs from the Hipparcos Catalog, and we made a literature survey of the spectroscopic binaries among the sample. We then investigated the overall binary frequency of the sample and the orbital characteristics of the known binaries. Binaries are common among O stars in clusters and associations but less so among field and especially runaway stars. There are many triple systems among the speckle binaries, and we discuss their possible role in the ejection of stars from clusters. The period distribution of the binaries is bimodal in log P, but we suggest that binaries with periods of years and decades may eventually be found to fill the gap. The mass ratio distribution of the visual binaries increases toward lower mass ratios, but low mass ratio companions are rare among close, spectroscopic binaries. We present distributions of the eccentricity and longitude of periastron for spectroscopic binaries with elliptical orbits, and we find strong evidence of a bias in the longitude of periastron distribution.

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