COMMISSION 27 OF THE I. A. U.
        INFORMATION BULLETIN ON VARIABLE STARS
                    Number 1182
                                   Konkoly Observatory
                                   Budapest
                                   1976 October 4



          MINIMA AND THE VISUAL LIGHT CURVE OF
           THE ECLIPSING BINARY RV PISCIUM


  The star RV Psc is an interesting Algol-system (alpha_1900=1h14m06s,
delta_1900= 30d40', 11.3m - 12.0m, F8), but not a classical Algolid, with
the very short period P = 13h17m45s and both minima are almost
equal. No period changes were observed (Ahnert 1975). Maybe the
components of RV Psc are subdwarfs (luminosity class VI) ?
  This paper contains the results of visual observations of
RV Psc made in the year 1936 at the island Hios (Greece) using
the 203 mm Expedition refractor. The observations were collected 
by Szafraniec (1962), but not elaborated as yet.
  The following comparison stars were used:
  a) a_1900  = 1h13m41s, delta_1900= +30d46.6',      m_v = 11.55m
     a_1900  = 1 13 46,  delta_1900= +30 42.5,       m_v = 11.90.

  Table 1 gives primary and secondary minima determined by the
tracing-paper method. The consecutive columns contain heliocentric 
time of minimum, kind of minimum, limit of error, number of
points n and O - C.
                      Table 1
             JD hel.      Min. Lim.error   n    O-C

           2428347.5065d  I   +-0.0015d   18  +0.0017d
           2428362.4620   I      .0015    33  -0.0006
           2428367.4485   I      .0015    27  +0.0000
           2428372.4405   I      .0020    13  +0.0061
           2428390.4405  II      .0015    20  +0.0014
           2428391.5500  II      .0020    11  +0.0029

  The values of O-C were obtained according to the elements given 
by Ahnert (1975):
                            
           Min. I JD hel. = 2424381.480d\ 
                                          +0.55399145 E.
           Min.II JD hel. = 2424381.757 /

  The Figure presents the mean visual light curve of the eclipsing 
binary RV Psc.
  Further observations, spectroscopic and photometric, are needed 
to explain the physical nature of this eclipsing system. 

                        [FIGURE 1]


                          T. Z. DWORAK
                          K. KORDYLEWSKI




References:
Ahnert, P. 1975, IBVS, No. 978
Szafraniec, R. 1962, Acta Astr.Suppl. 5, 719