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The eclipsing binary BW Draconis
The eclipsing binary BW Dra has been observed during September 1980 andMay and June 1981 with a 48-inch reflector, using a two-beam multimodenebular-stellar photometer with B- and V-filters. The star SAO 166029 istaken as a point for comparison. Attention is presently given to the B-and V-lightcurves obtained.
| Photoelectric observations of BV Draconis
The two B and V light curves of the close eclipsing binary BV Draconiswere obtained with a two-beam, multi-mode, nebular-stellar photometer,using the star SAO 166029 for comparison. It is found that both B and Vmaxima are equal in the two curves, and that the depth of the minima isnearly the same. Since there are many observational points for thephases from 0.0 to 0.55, both minima as well as the maximum followingprimary minimum are well observed. The dispersions obtained are small inthe B curve and large in the V curve.
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