COMMISSION 27 OF THE I. A. U.
          INFORMATION BULLETIN ON VARIABLE STARS
                      Number 2702

                                   Konkoly Observatory
                                   Budapest
                                   2 April 1985

                                   HU ISSN 0374 - 0676


        BD+61 deg 277 CONFIRMED AS AN ECLIPSING BINARY STAR


   The star BD+61 deg 277 was noted to be an eclipsing binary by Soloviev
(1944), who found a preliminary period of 2.4 d. Apparently no further
observations have been made of this star. BD+61 deg 277 was monitored on 10
nights during the 1983-1984 observing season and on 20 nights during the
1984-1985 observing season with the 41-cm reflector of the Morgan-Monroe
Station of the Goethe Link Observatory. Differential measurements were
made using BD+61 deg 282 as a comparison star. The photometer employed a 1P21
photomultiplier tube cooled with dry ice and standard B and V filters.
Observations of standard stars for determining extinction and transformation
coefficients were made on two nights during the Autumn of 1984. From these
it was found that Vmax = 9.5 and (B-V) = +.58.


                             [FIGURE 1]



   BD+61 deg 277 was observed to be in eclipse on several nights, but the 2.4 d
period did not fit the observations well. Plots of the observations were generated
using various values of the period. The best fit occurred with a period of
6.1622 d. The accompanying figure shows the observations folded on this period.
The primary eclipse was found to be .45 mag deep and the secondary .25 mag deep.The
duration of secondary eclipse is 1.7 d. The sparseness of observations near
primary eclipse made it impossible to determine a time of primary minimum light
with any precision. It was possible to estimate the time of minimum light for
one secondary eclipse, and this epoch may be used to predict future eclipses:
           HJD Min I = 2446024.969 + 6.1622(E + .5).
Soloviev published 3 times of minimum light determined from photographic
observations. It was not possible to reconcile these epochs of minimum light
with the period determined in this study.





                             DANNY R. FAULKNER

                             Astronomy Department
                             Swain West 319
                             Indiana University
                             Bloomington, IN 47405 U.S.A.





  Reference:
  Soloviev, A. 1944 Astronomical Circulars No. 34.