COMMISSION 27 OF THE I. A. U.
             INFORMATION BULLETIN ON VARIABLE STARS
                         Number 3060


                                               Konkoly Observatory
                                               Budapest
                                               7 August 1987

                                               HU ISSN 0374-0676


               THE 1986 LIGHT CURVES OF UV PISCIUM

  Based on photographic observations, the light curve of UV Psc was first
published by Huth (1959). Hall (1976), included the system in the short-
period group of RS CVn-type binaries. The spectroscopic record of UV Psc is
due to Popper (1969) and the system is listed as a double-line binary with
emission from both components present in the H and K lines of Ca II. The
photoelectric observations of the system were made by several investigators.
According to his light curve analysis Sadik (1979) stated that the irregularities
in the light curve were caused by a locally hotter (rather than cooler)
region.
  Two-colour photoelectric observations of UV Psc were carried out from
November 10 to November 20, 1986 at the Ege University Observatory with the
48 cm Cassegrain telescope equipped with an EMI 9781A photomultiplier. B and
V filters of the standard UBV system were utilized to secure the observations,
BD +6 191 and BD +6 197 were used as comparison and check stars, respectively. 
The differential magnitudes in the sense variable minus comparison
were corrected for atmospheric extinction and the times of the individual 
observations were reduced to the Sun's centre. The phases of the individual 
observations were calculated with the new light elements given by Ibanoglu(1987)
as,

     Min I =J.D. Hel. 2444 932.2985 + 0.86104771dE.
                               +/-2        +/-11

  In Figure 1, B and V light curves of UV Psc obtained in the observing season
of 1986 are presented. A continuous light variation due to the wave-like 
distortion can be easily recognized, except for the phase interval 0.065-0.225
for the blue light. The wave minimum seems to be located just at the secondary
minimum of the light curve. As in the light curves of all other RS CVn type
binaries, the location of the minimum of the wavelike distortion is shifted 
towards the decreasing orbital phases in the case of UV Psc, with a period of
roughly 1.5-2.0 years.


                               [FIGURE 1]

      Figure 1: B and V light curves of UV Psc obtained in 1986.


  The light curves of the system obtained in 1986 can be considered quiet
if the fluctuations between the phase interval 0.475-0.525 are ignored. For
the observing season of 1982, however, the light curves of the system in both
colours proved to be considerably fluctuating (Ibanoglu, 1987).
  The observations of the system will be carried out in the coming observing
season.



V. KESKIN, M.C. AKAN, C. IBANOGLU,
     Z. TUNCA and S. EVREN

  Ege University Observatory
  Bornova, Izmir/TURKEY


References;
Hall, D.S.: 1976, Proc. of IAU Coll. No.29 (Budapest), Part 1, 287. [BIBCODE 1976ASSL...60..287H ]
Huth, H.: 1959, Mitteilungen uber veranderliche Sterne, Nr. 424.
Ibanoglu, C.: 1987, Astrophys. Space Sci., (in press). [BIBCODE 1987Ap&SS.139..139I ]
Popper, D.M.: 1969, B.A.A.S., 1, 257. [BIBCODE 1969BAAS....1R.257P ]
Sadik, A.R.: 1979, Astrophys. Space Sci., 63, 319. [BIBCODE 1979Ap&SS..63..319S ]