A New Light Curve and Analysis of the Long Period Eclipsing Binary BF Draconis

Details A New Light Curve and Analysis of the Long Period Eclipsing Binary BF Draconis A New Light Curve and Analysis of the Long Period Eclipsing Binary BF Draconis

Jan 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...19312403w&link_type=abstract

American Astronomical Society, 193rd AAS Meeting, #124.03; Bulletin of the American Astronomical Society, Vol. 31, p.668

Astronomy and Astrophysics

Astronomy

Scientific paper

The star BF Draconis was found to be an eclipsing binary by Strohmeier, Knigge and Ott (1962) and originally thought to be an Algol-type system with a period of 5.6 days. A spectrographic study by Imbert (1985) showed that the period was actually double this value and that the system consisted of two well-separated, almost-equal F-type stars in elliptical orbit. Diethelm, Wolf and Agerer (1993) later published a preliminary light curve of this system showing minima of unequal depth and width with a displaced secondary, confirming the elliptical orbit but disagreeing with Imbert on the specific orbital parameters. As a part of our long-term program of obtaining improved light curves of double-lined spectroscopic and eclipsing binaries, we have observed BF Draconis for the past four years using the 0.4 meter telescope at the Baker Observatory of Southwest Missouri State University. Complete light curves in the Cousins BVRI passbands have been obtained with our Photometrics CCD system, and a new model and orbital parameters for the binary have been determined using the Wilson-Devinney program. This research has been supported by NSF Grants AST-9315061 and AST-9605822 and NASA Grant NGT5-40060.

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