COMMISSION 27 OF THE I. A. U. INFORMATION BULLETIN ON VARIABLE STARS Number 3404 Konkoly Observatory Budapest 12 December 1989 HU ISSN 0374 - 0676 1989 LIGHT CURVES OF BH VIRGINIS BH Virginis (BD-0d2769,HD121909) is a double-lined spectroscopic eclipsing binary with cool components. The spectral types of the components have been determined as GOV+G2V by Abt (1965) and as F8IV-V+G2V by Koch(1967). Having late type magnetically active components, the system's total light at maxima and/or minima is expected to vary in time (Hoffmann, 1982; Budding and Gimenez, 1982). It has been observed photometrically by Kitamura et al. (1957), Koch (1967), Sadik (1978), Hoffmann (1982) and Scaltriti et al.(1985). In addition to ellipticity and reflection effects outside the eclipse phases, an irregular fluctuation as a characteristic property of RS CVn type systems has been noted as early as 1957 by Kitamura et al. (1957). Scaltriti et al. (1985) have noted by comparing the existing observations that the distortion wave is variable and migrates in time, while Budding and Zeilik (1987) found a distortion wave of about same shape with two minima at about the same phases from Sadik (1978) and Scaltriti et al.'s (1985) data. True interpretation of the light variations at different time scales requires a continuous monitoring of the binary. Thus, we have included BH Vir in our program of the photometric observations of short period binaries. The present observations of BH Vir were made on seven nights in 1989 using an EMI 9789QB photomultiplier attached to the 30 cm Maksutov telescope of the Ankara University Observatory. The differential observations in U, B and V colors were made with respect to the comparison star BD-0d2770. Altogether 188, 190 and 187 differential magnitudes of BH Vir in V, B and U bandpass, respectively, [FIGURE 1] Figure 1. The UBV observations of BH Vir in 1989 were obtained. The individual differential magnitude determinations were corrected for differential atmospheric extinction. The observations (in the sense variable minus comparison) are shown in Figure 1 together with the color curves. The phases were calculated by using the light element from GCVS (1985), as Hel. JD Min I = 2443230.609 + 0.816877161 * E Two primary and one secondary eclipse minima have been secured during the observations. The new times of the minima are given in Table 1. Table 1. The new times of minima of BH Vir Hel. Min. Filter E O-C Remark 2447600+ 15.5743 +-0.0006 U 11640 0.0093 Min.I 15.5732 +-0.0005 B 11640 0.0082 Min.I 15.5734 +-0.0013 V 11640 0.0084 Min.I 20.4754 +-0.0018 U 11646 0.0092 Min.I 20.4738 +-0.0004 B 11646 0.0076 Min.I 20.4738 +-0.0013 V 11646 0.0076 Min.I 58.4604 +-0.0027 U 11692 0.0097 Min. II 58.4580 +-0.0018 B 11692 0.0073 Min. II 58.4579 +-0.0013 V 11692 0.0072 Min. II ETHEM DERMAN AYVUR AKALIN OSMAN DEMIRCAN Ankara University Observatory Science Faculty, Astronomy Department Tandogan, 06100 Ankara / Turkey References: Abt, H. A. : 1965, Publ. Astron. Soc. Pacific, 77, 367. [BIBCODE 1965PASP...77..367A ] Budding, E., Gimenez, A. : 1982, Proceedings of Third European IAU Conference, ESA SP-176, p. 169. [BIBCODE 1982ESASP.176..169B ] Budding, E., Zeilik, M. : 1987, Astrophys. J., 319, 817. [BIBCODE 1987ApJ...319..827B ] Hoffmann, M. : 1982, Astron. Astrophys. Suppl. Ser., 47, 561. [BIBCODE 1982A&AS...47..561H ] Kitamura, M., Nakamura, T., Takahashi, C. : 1957, Publ. Astron. Soc. Japan, 9, 191. [BIBCODE 1957PASJ....9..191K ] Koch, R. H. : 1967, Astron. J., 72, 411. [BIBCODE 1967AJ.....72..411K ] Sadik, A. R. : 1978, Ph. D. Thesis Univ. of Manchester. [BIBCODE 1978PhDT.......296S ] Scaltriti, F., Cellino, A., Busso, M. : 1985, Astron. Astrophys., 149, 11. [BIBCODE 1985A&A...149...11S ]