COMMISSION 27 OF THE I. A. U.
       INFORMATION BULLETIN ON VARIABLE STARS
                    NUMBER 578

                                Konkoly Observatory
                                Budapest
                                1971 September 6


  UBV PHOTOMETRY OF THE SUSPECTED VARIABLE BD +18d4586

     Recently Moore (1969) has suspected that the star
BD +18d4586 is a variable with an amplitude of about 0.5m
and a semi-regular period of a few weeks. We therefore added
this star to our program during an observing session at the
Kitt Peak National Observatory in June 1970.
     Altogether we obtained 22 observations on eight
nights during a two week interval, using the No. 4 16-inch
reflector equipped with a 1P21 photomultiplier which was
refrigerated with dry ice. The three-color observations were
made differentially with respect to the comparison star
BD +18d4602. In addition we observed this comparison star
differentially with respect to the check star BD +19d4489.
All magnitudes were corrected for differential extinction
and transformed differentially to the UBV system.
     Nightly averages for each color were formed and the
resulting rms deviations are listed in the table below.


---------------------------------------------------
                         V          B          U
---------------------------------------------------
18d4586 vs. 18d4602   +-0.02m    +-0.02m    +-0.04m
19d4489 vs. 18d4602   +-0.01     +-0.02     +-0.03
---------------------------------------------------


From these results it is obvious that, although the scatter
is about 0.01m larger for the suspected variable than for
the check star, there is certainly no evidence for the large
variability suspected by Moore. Although it is always 
impossible to be certain in cases like this (for instance the
star could be an eclipsing binary which Moore occasionally
observed inside eclipse and we always observed outside 
eclipse), our data lead us to believe that BD +18d4586 is not
a variable star.

                   R.C. TATE and E.W. BURKE, Jr.
                    King College Observatory
                      Bristol, Tennessee
                          U.S.A.

Reference:
Moore, P. 1969, I.A.U. Inf.Bull.Var.Stars, No 385.




             NOTES ON VARIABLES

     WX Hydri: Estimations on Sonneberg patrol plates of
the southern sky confirm the statements given in IAU Circular
No. 2348. Two maxima were observed (J.D. 242 8846 and
243 4240). The rise to maximum is rather steep:

         242 8841.3   13.47m phg.
               42.4   12.81
               43.3   12.78
               44.4   12.46
               45.3   12.43

For details see forthcoming number of MVS,


     Star No. 9 in the Region of Cygnus XR-2: The variability 
of star no. 9 of Giacconi's note (ApJ 148, L 129)
is confirmed on Sonneberg photovisual patrol plates. The
character of variability remains as yet unknown.


     V 1057 Cygni: The star is still near maximum light
(10.8m phg.) on Sonneberg patrol plates of J.D. 244 1134.4,
1155.5, 1179.5, and 1180.4 (1971 July-August).




                       EBERHARD SPLITTGERBER
                          Halle/Saale
                       Adam-Kuckhoff-Str. 2
                            DDR