COMMISSION 27 OF THE I. A. U.
          INFORMATION BULLETIN ON VARIABLE STARS
                      Number 2782

                                        Konkoly Observatory
                                        Budapest
                                        27 August 1985

                                        HU ISSN 0374 - 0676


           PHOTOELECTRIC OBSERVATIONS OF ER VULPECULAE


  The peculiar eclipsing binary ER Vul was discovered spectroscopically by
Northcott and Bakos (1956). The photoelectric observations made by Northcott
and Bakos (1967) revealed its light variation. When the star was included in
the list of short period group of the RS CVn binaries by Hall (1976) it called
more attention. The light curve variations were discussed by Al-Naimiy (1978),
Hrivnak (1982) and Kadouri (1981). The H and K emissions of singly ionised
calcium were observed by Bond (1970).
  The system ER Vul was observed at Ege University Observatory from 1981 to
1985. The observations were made with the 48 cm Cassegrain reflector, which
was equipped with an unrefrigerated EMI 9781 A photomultiplier with B and
V filters of the standard UBV system. BD+27deg 3946 was used as the comparison
star.

            Table I
            The times of minima of ER Vul.

   Hel J.D.    O-C       E         Colour
   2440000+
   5900.3536 +0.0028d    8191      b
       .3522   .0014     8191      v
   5901.4043   .0064     8192.5    b
       .4036   .0057     8192.5    v
   5902.4481   .0030     8194      b
       .4468   .0017     8194      v
   5933.5126   .0023     8238.5    b
       .5119   .0016     8238.5    v
   5939.4465   .0024     8247      b
       .4472   .0031     8247      v
   6004.3776   .0108     8340      b
       .3808   .0140     8340      v
   6235.4368   .0008     8671      b
       .4406   .0046     8671      v
   6241.3738   .0040     8679.5    b
       .3712   .0014     8679.5    v
   6248.3577   .0070     8689.5    b
       .3513  +.0006     8689.5    v
   6256.3774  -.0014     8701      b
       .3806  +.0018     8701      v


  The times of minima derived from the observations of last two years are
given in Table I. The O - C residuals are the differences between
observed and predicted times of minima according to the ephemeris:

         Min I = JD Hel. 2440 182.2621 + 0.69809409d.E.

  The star will be monitored again in the coming months and the light
curves will be presented and discussed elsewhere.





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

                        Ege University Observatory
                        Bornova - Izmir
                        Turkey





References :

Al-Naimiy, H.M.: 1978, IBVS No. 1481.
Bond, H.E.: 1970, Pub.A.S.P. 82, 321. [BIBCODE 1970PASP...82..321B ]
Hall, D.S.: 1976, Proc.of I.A.U. Coll. No. 29 (Budapest), Part. 1, 287. [BIBCODE 1976ASSL...60..287H ]
Hrivnak, B.J.: 1982, 159 th meeting of the American Astronomical Society,
        Boulder, Colorado.
Kadouri, T.H.: 1981, IBVS. No. 2057.
Northcott, R.J., and Bakos, G.A.: 1956, Astron.J. 61, 188. [BIBCODE 1956AJ.....61..188N ]
Northcott, R.J., and Bakos, G.A.: 1967, Astron.J. 72, 89. [BIBCODE 1967AJ.....72...89N ]