COMMISSION 27 OF THE I. A. U. INFORMATION BULLETIN ON VARIABLE STARS Number 3403 Konkoly Observatory Budapest 12 December 1989 HU ISSN 0374 - 0676 1988 LIGHT CURVES OF RX HERCULIS RX Her (HD 170757, GC 25274) is a detached eclipsing binary with algol type light curves. It was listed by Popper (1959) as one of four early spectral type eclipsing binaries with well determined properties. Wood (1948) obtained one unfiltered light curve and determined a solution using the Russell-Merrill method. Other light curves obtained were never solved because no significant differences were noticed between new and old light curves (Popper, 1959). Olson(1975) and Hill and Hilditch (1975) observed the system at five different phases in Stromgren filters. From these observations the C index indicates a B9.5 spectral type, while the M index for both primary and secondary stars shows nothing peculiar in the metal abundance (Jeffreys, 1980). Jeffreys (1980) obtained a V light curve and determined a solution using Wood's (1971) WINK computer model. He found that RX Her is a binary system with similar components (B9.5 primary and A0 secondary). He also found some asymmetry during ingress of the secondary due to a small eccentricity (e = 0.022). We obtained new differential photoelectric observations in each U, B, V filters during May and August 1988. An EMI 9789QB photomultiplier attached to the 30 cm Maksutov telescope of the Ankara University Observatory has been used to secure the data. Differential observations in three colors were made with respect to the comparison star BD+12d3547. BD+11d3518 was used as the check star. The differential brightness measurements of the comparison with respect to the check star were found to be sensibly constant during the observations. The individual differential brightness determinations were corrected for differential atmospheric [FIGURE 1] Figure 1. The UBV observations of RX Herculis. extinction. The observations in the sense variable minus comparison are plotted in Figure 1 together with color curves. The light elements used in phase calculation were given in GCVS 1985 as Hel. JD Min I = 2433170.398 + 1.7785724d*E. Table 1. The new times of minima of RX Her Hel.Min. No Filter E O-C Remark 2447300+ of obs 39.3930 +- 0.0020 11 U 7966 -0.0020 Min. II 39.3947 +- 0.0009 16 B 7966 -0.0004 Min. II 39.3946 +- 0.0010 16 V 7966 -0.0004 Min. II 47.3989 +- 0.0006 15 U 7971 +0.0003 Min. I 47.3991 +- 0.0008 15 B 7971 +0.0005 Min. I 47.4003 +- 0.0013 13 V 7971 +0.0017 Min. I 71.4032 +- 0.0031 9 U 7984 -0.0062 Min. II 71.4072 +- 0.0002 9 B 7984 -0.0021 Min. II 71.4078 +- 0.0030 11 V 7984 -0.0015 Min. II 79.4139 +- 0.0004 32 U 7989 +0.0010 Min. I 79.4141 +- 0.0003 30 B 7989 +0.0012 Min. I 79.4139 +- 0.0005 32 V 7989 +0.0010 Min. I 88.3067 +- 0.0009 20 U 7994 +0.0009 Min. I 88.3059 +- 0.0005 20 B 7994 +0.0001 Min. I 88.3068 +- 0.0013 20 V 7994 +0.0010 Min. I During the observations we secured three primary and two secondary minima. The new minimum times (see Table 1 ) confirm the apsidal motion and thus eccentric orbit of the system. We thank to B. Gürol for the generous help during the observations and their reductions. OSMAN DEMIRCAN ETHEM DERMAN Ankara University Observatory Science Faculty, Tandogan 06100 Ankara / Turkey References: Hill G., Hilditch, R. W.: 1975, Mem. R. Astron. Soc., 79, 123. [BIBCODE 1975MmRAS..79..101H ] Jeffreys, K. W. : 1980, Astron and Astrophys. Suppl., 42, 285. [BIBCODE 1980A&AS...42..285J ] Olson, E. C.: 1975, Astrophys. J., Suppl., 29, 43. [BIBCODE 1975ApJS...29...43O ] Popper, D. M.: 1959, Astrophys. J., 129, 659. [BIBCODE 1959ApJ...129..659P ] Wood, D. B.: 1971, Astron. J., 76, 701. [BIBCODE 1971AJ.....76..701W ] Wood. F. B.: 1948, Astrophys. J., 110, 463. [BIBCODE 1949ApJ...110..465B ]