COMMISSION 27 OF THE I. A. U. INFORMATION BULLETIN ON VARIABLE STARS Number 1029 Konkoly Observatory Budapest 1975 August 7 PHOTOELECTRIC PHOTOMETRY OF WY CANCRI WY Cancri was discovered to be variable by Hoffmeister in 1948 and recognized as an Algol-type eclipsing binary by Kippenhahn in 1953. Chambliss (Astron.J. vol. 70, p. 741, 1965) published the first photoelectric investigation of this system. When his observations, which were made in 1969-65, were combined with earlier ones the following ephemeris was obtained: Hel. Min I =JD 2426352.3895 + 0.82937122d E +-22 +-16 p.e. Subsequently Ahnert (MVS Sonneberg vol. 6, p. 107, 1973) obtained a similar ephemeris and noted that the period of WY Cancri has remained constant for the past 40 years. In January, 1975 the author obtained one additional time of minimum light using a 16-inch telescope at Kitt Peak National Observatory. When this time is combined with those previously published, the following ephemeris is obtained: Hel. Min I =JD 2426352.3888 + 0.82937126d E +-17 +-11 p.e. This ephemeris is essentially identical with the one previously given as the differences between them are much smaller than their respective probable errors. Observed times of minimum light of WY Cancri are listed in the following table. Observations made on the same night have been averaged. ---------------------------------------------- Hel. JD E Method Wt. O-C ---------------------------------------------- 2426352.392 0 pg 1 +0.0032d 396.352 53 pg 1 +0.0066 608.644 309 pg 1 -0.0205 7898.341 1864 pg 1 +0.0042 8607.463 2719 pg 1 +0.0138 8622.377 2737 pg 1 -0.0009 2436612.534 12371 pg 1 -0.0066 7346.533 13256 v 3 -0.0012 352.341 13263 v 3 +0.0012 356.485 13268 v 3 -0.0017 366.439 13280 v 3 -0.0001 376.393 13292 v 3 +0.0014 667.504 13643 v 1 +0.0031 2437707.310 13691 v 1 -0.0007 731.362 13720 v 1 -0.0005 8091.309 14154 v 1 -0.0006 739.8779 14936 pe 10 0.0000 788.8111 14995 pe 10 +0.0003 794.6169 15002 pe 10 +0.0005 847.6959 15066 pe 10 -0.0003 854.325 15074 v 1 -0.0062 9223.401 15519 v 1 -0.0004 238.314 15537 v 1 -0.0160 490.461 15841 v 1 +0.0021 932.518 16374 v 1 +0.0042 2440988.308 17647 v 1 +0.0046 1041.384 17711 v 1 +0.0008 1055.484 17728 v 1 +0.0015 1765.4225 18584 pg 3 -0.0018 2433.8985 19390 pe 10 +0.0010 ----------------------------------------------- The star BD + 27d1701 was used as a comparison, while BD + 28d1672 was used as a check star. The magnitudes and colors obtained for these stars are as follows: --------------------------------------------- V B-V U-B --------------------------------------------- WY Cancri (max.) 9.51 +0.72 +0.17 WY Cancri (pri.) 10.14 +0.79 +0.23 BD + 27d1701 10.00 +0.64 +0.15 BD + 28d1672 9.61 +0.98 +0.88 --------------------------------------------- The depths of the primary minimum are 0.63m,0.70m and 0.76m in yellow, blue, and ultraviolet,respectively. A faint star is observed about 20"N of WY Cancri. The approximate magnitudes and colors of this star are V = 12.8, B-V = + 0.6, and U-B = +0.1. The colors and magnitudes given for WY Cancri exclude any contribution from this star, but all of the observations made by this investigator in 1964-65 include it as a 72" diaphragm was used at that time. Additional U,B,V photoelectric observations of WY Cancri are planned. CARLSON R. CHAMBLISS Dept. of Physical Sciences Kutztown State College Kutztown, Penna., U.S.A.