COMMISSION 27 OF THE I. A. U.
         INFORMATION BULLETIN ON VARIABLE STARS
                     Number 1381

                                    Konkoly Observatory
                                    Budapest
                                    1978 January 18




           UV Psc - A SHORT PERIOD RS CVn STAR




    UV Psc has been listed by Hall (1976) in Table 3 (the Short-
Period Group) of his paper on the RS CVn binaries. The inclusion
comes from the discussion of Oliver (1974) who argued in favour
of a subgiant companion to the primary G2V star. Oliver's light
curve was itself incomplete outside the minima, while Carr's
light curve (private communication cited by Oliver), though
showing a greater coverage outside of the minima, appears to be
incomplete around the primary minimum.
    Light curves of the system in B and V colours were obtained 
at the Kottamia station of Helwan Observatory (Egypt) during
the first two weeks of November 1977. The desert location of the 
observatory offers special advantages for high-grade photometry:
The main comparison star was BD+6d 197. The stars BD+6d 195
BD+6d 191 were used for occasional checks.
    The photometer and associated equipment used in this work
have been described by Mikhail (1968) and Awadallah (1975).
    The reduction procedure follows along the lines discussed
by Hardie (1962), and has been extensively automated allowing
the digitization measurement, computer data processing and
graphical output systems of the University of Manchester Regional 
Computer Centre to be made use of.
    Preliminary results are shown in the diagrams below.
    The essential asymmetry of the out-of-eclipse portions is
obvious, though it is not yet certain whether this corresponds
strictly to a "wave" in the sense discussed by Hall (1976). The
asymmetry can also be seen to be more pronounced in the B than
the V light curve. A similar asymmetry in the same sense is 
indicated in Carr's light curve, though it is not obvious in the
observations of Oliver.
    Further observations of the system are planned for January
1978 to confirm the reality of the asymmetry and other features.
    The author would like to make special mention of the help
and cooperation of the staff of Helwan Observatory during this
program.





                           A. R. SADIK
                           University of Manchester,
                           Department of Astronomy,
                           Manchester, England


References:
Awadallah, N.S. 1975, M.Sc. Thesis, University of Cairo,
        (unpublished)                                     
Hall, D.S. 1976, Proc. of I.A.U. Coll. No. 29 (Budapest), Part 1,
        p. 287, Reidel, Dordrecht [BIBCODE 1976ASSL...60..287H ]
Hardie, R.H. 1962, in Astronomical Techniques, p.178, ed. W.A.
        Hiltner, Chicago [BIBCODE 1964aste.book..178H ]
Mikhail, J.S. 1968, Icarus, 8, 117 [BIBCODE 1968Icar....8..117S ]
Oliver, J.P. 1974, Ph.D. Thesis, University of California,
        Los Angeles, (unpublished) [BIBCODE 1974PhDT.........1O ]


                         [FIGURE 1]
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                         [FIGURE 3]