COMMISSION 27 OF THE I. A. U.
       INFORMATION BULLETIN ON VARIABLE STARS
                    NUMBER 408

                             Konkoly Observatory
                             Budapest
                             1969 November 27


           THE VARIABILITY OF BV 516

      The eclipsing binary BV 516 (HD 124195) was given
the following ephemeris by Schoffel and Kohler (IBVS no.77,
1965):

         Min. I = JD 2438524.410 + 1d49008

     Photoelectric observations of BV 516 were made by
the present author at the Mount John University Observatory
in New Zealand on 10 nights during April, May, June, and
July of 1966. The star HD 122844 was used as a comparison.
Four times of minimum light were obtained. Combining these
with the previously published times of minimum light, the
following ephemeris was obtained:

         Min. I = JD 2438524.4069 + 1d490096 E.
                        +- 96     +- 20 p.e.

The individual times of minimum light were as follows:

Hel. JD          E   O-C       Method   Obs.*
2438524.303      0   -0d0139   pg       S,K
530.340          4   -0.0272   pg       S,K
548.291         16   +0.0428   pg       S,K
2439262.0070   495   +0.0025   pe       Ch
284.9801       497   -0.0046   pe       Ch
282.8659       509    0.0000   pe       Ch
291.8084       515   +0.0019   pe       Ch
*S, K = Schoffel and Kohler;  Ch = Chambliss

In New Zealand about 800 photoelectric observations
of BV 516 were obtained in yellow and in blue light (400 in
each color). BV 518 is a Beta Lyrae type eclipsing binary.
The primary minimum is about 0m58 deep in yellow light, and
the secondary is about 0m25 deep in the same color. The
respective values for blue light are 0m58 and 0m24. However,large 
fluctuations were found in the light curve, particularly 
in the portions outside of the eclipses. These
variations could be either intrinsic, or else, due to
variability in the comparison star, HD 122844.

      In July of 1969 photoelectric observations were made
at the Cerro Tololo Inter-American Observatory in Chile of
the star HD 122844 and a check star, HD 119727, to see if
the former might be variable. No variations were found. Thus
it appears that the large scatter found in the observations
of BV 516 is due in part to intrinsic fluctuations in the
light curve of BV 516.
      The following magnitudes and colors were obtained
for the stars mentioned:

                 		  V   B-Y    U-B   Spectrum

BV 516 (at max.)	      5.98 +0.10  ...	   B9
HD 119727               6.45 +0.12 +0.09     AO
HD 122844               6.17 +0.25 +0.18     A3


The spectral types are those given in the Henry Draper
Catalogue.
      Further photoelectric observations will be necessary
in order to determine the orbital elements of BV 516 and the
nature of the fluctuations in its light curve.



November 21, 1969      CARLSON R.CHAMBLISS
                   Georgetown College Observatory
                     Washington, D.C., U.S.A,



              NOVA IN SAGITTARIUS

       The Nova, reported in I.A.U. Information Bulletin
on Variable Stars, Number 389, is in the Perth Astrographic
Zone. The star is not shown on plates of the area exposed
in 1902,1904,1910 and 1914, with limiting magnitude 13m
to 14m. It is shown on a repeat plate exposed 1969 August
28.523 U.T. By visual comparison with other stars on the
plate, which have magnitudes in the Yale Catalogue, we
estimate a photographic magnitude of 9m7+-0m1.
                November 18,1969
                                   M.P.CANDY
                                Perth Observatory, Bickley,
                                Western Australia,6076.