COMMISSION 27 OF THE I. A. U. INFORMATION BULLETIN ON VARIABLE STARS Number 1767 Konkoly Observatory Budapest 1980 April 3 ELEMENTS FOR CSV 8853=Wr 136 CSV 8853=Wr 136 (alpha1900: 23h22m19s, delta1900:+45d01') was discovered photographically by R. Weber (1963). He classified the star as a probable cepheid variable. One of us (A.G.) set out to determine the elements of variability of CSV 8853 visually in the summer of 1979, using his 20 cm Newton reflector. Very soon it became evident, that the period of variation was rather short, amounting to some 5 hours. Table I lists all the visually determined times of maximum light along with the number of observations. From these observations the following preliminary elements were deduced, employing standard least squares methods: (1) JD max hel = 2444065.462+0.190429*E. O-C values and E in Table I refer to these elements. Table I Visual times of maximum for CSV 8853 JD max hel O-C E n 2400000+ 44065.4544 -0.0086 0 9 069.4672 +0.0048 21 17 070.4173 +0.0027 26 13 070.5902 -0.0148 27 7 072.5007 -0.0087 37 20 073.4550 -0.0067 42 11 076.5128 +0.0039 58 25 077.4643 +0.0032 63 24 078.4157 +0.0024 68 18 081.4653 +0.0049 84 15 082.4103 -0.0023 89 15 087.3677 +0.0035 115 18 118.3937 -0.0130 278 8 133.4463 -0.0055 357 6 143.3472 -0.0078 409 9 [FIGURE 1] Figure 1. Photoelectric V- and B-V-curve of CSV 8853 obtained with the Basel University photometer attached to the 1m reflector on the Gronergrat, Switzerland. Circlets denote observations obtained on JD 2444081, crosses observations obtained on JD 2444087. Table II Photoelectric observations of CSV 8853 t_obs phase V B-V 44081.4640 0.0061 11.230 0.590 44087.3770 0.0571 11.190 0.640 44081.4800 0.0901 11.210 0.670 44087.3920 0.1358 11.270 0.600 44081.4950 0.1689 11.270 0.610 44087.4060 0.2094 11.320 0.620 44081.5070 0.2319 11.330 0.630 44087.4170 0.2671 11.360 0.660 44081.5210 0.3055 11.460 0.620 44087.4250 0.3091 11.440 0.700 44087.4310 0.3406 11.520 0.690 44081.5360 0.3842 11.600 0.570 44087.4450 0.4142 11.650 0.670 44081.3580 0.4495 11.750 0.550 44081.5510 0.4630 11.820 0.630 44087.4680 0.5349 11.740 0.550 44081.5680 0.5523 11.720 0.650 44081.3800 0.5650 11.730 0.590 44087.4810 0.6032 11.580 0.680 44081.5820 0.6258 11.600 0.580 44087.4910 0.6557 11.480 0.630 44081.4010 0.6753 11.460 0.680 44087.5070 0.7397 11.340 0.640 44081.4160 0.7541 11.320 0.640 44087.5210 0.8133 11.250 0.680 44081.4360 0.8591 11.240 0.660 44087.5350 0.8868 11.190 0.680 44087.3500 0.9153 11.260 0.610 44081.4500 0.9326 11.220 0.660 44087.5490 0.9603 11.200 0.620 In order to check the elements and to secure a photoelectric light-curve, one of us (R.D) observed CVS 8853 during two nights in the summer of 1979, covering the whole cycle in both cases. We used the single channel RGUBV-photometer of Basel University attached to the 1 meter reflector of Gornergrat station, Switzerland (3100 m/M) operated by "Stiftung Hochalpine Forschungsstationen Jungfraujoch und Gornergrat". Transformation into the standard Johnson UBV-system was obtained by repeated observations of standard stars. Table II lists the V magnitudes as well as the B-V colours. They were all reduced differentially by comparing the variable with comparison star c in Weber's chart, lying some 3' south of CSV 8853 (V=11.55+-0.02, B-V=+0.61+-0.03). Due to the close proximity of the variable and the comparison star, the use of mean extinction coefficient was appropriate. The internal errors of a single observation amounts to 0.02 in V and 0.03 in B-V. R. DIETHELM Astronomical Institute of Basel University Switzerland A. GAUTSCHY Gontenschwil Switzerland Reference: Weber, R, 1963, I.B.V.S. No. 21