COMMISSION 27 OF THE I. A. U.
         INFORMATION BULLETIN ON VARIABLE STARS
                     Number 2840

                                     Konkoly Observatory
                                     Budapest
                                     27 December 1985

                                     HU ISSN 0374 - 0676


               1984 UBVRI PHOTOMETRY OF II Peg



  The II Peg (HD224085, SAO 091578) is a spectroscopic binary
with a spectral type K2-3IV-V, Rucinski (1977), considered to
be a member of RS CVn stars. As is well known, its light curves
are highly variable in amplitude, phase and mean light level,
Hartmann et al.(1979).
  Our observations were made during 14 nights, between
August and September 1984, from the Observatorio del Roque de
los Muchachos at La Palma (Canary Islands), using the People's
Photometer a two-channel photoelectric photometer and UBVRI
filters of Cousins system (1976) at the Cassegrain focus of
1 m JK Telescope, and on the Swedish 60 cm Cassegrain Telescope 
with a single channel photon counting photoelectric UBV
Johnson photometer.
  The stars SAO 091577 and SAO 091574 were used as comparison.
The nightly means of individual differential magnitudes (source-
comparison) in UBVRI are listed in Table I, as well the Julian
date of the observation.

                             Table I

J.Date     DeltaU    DeltaB  DeltaV   DeltaR   DeltaI
2445000+
936.712    -1.708   -0.971   -0.709   -0.682   -0.692
937.712    -1.614   -0.915   -0.661   -0.633   -0.642
938.712    -1.657   -0.969   -0.698   -0.672   -0.698
940.713    -1.701   -0.999   -0.745   -0.714   -0.737
945.712                      -0.762
951.723    -1.578   -0.965   -0.681
953.578    -1.648   -0.921   -0.687
954.713             -0.913   -0.708
955.578             -1.056   -0.801
955.713    -1.761   -1.052   -0.787
959.578    -1.676   -0.924   -0.702
960.713    -1.667   -0.951   -0.715
961.713    -1.713   -1.030   -0.779
966.599    -1.640            -0.647



                      [FIGURE 1]






   The results are also given in Figure 1, where the differential 
magnitude is plotted against the phase calculated using
the ephemerides of Rucinski (1977)

        JD = 2443033.10 + 6.724183d E

   From the light curves we observed two minima at about 0.26
and 0.97 phases with similar amplitude, approximately 0.15 mag.
These new observations are markedly different from those 
previously reported by Zeilik et al. (1982), Hall and Henry (1983)
Lines et al. (1983) and Henry (1983). If compared to the light
curve obtained by Nations and Ramsey (1981) it seems to show
some similitude since they found two maxima at 0.55 separation
in phase although of different amplitude.



            M.J. AREVALO, C. LAZARO and J.J. FUENSALIDA

            Instituto de Astrofisica de Canarias
            38071 La Laguna
            Tenerife, SPAIN


References:

Cousins, A.W.J.: 1976, Mem. Roy. Astron. Soc., 81, 25. [BIBCODE 1976MmRAS..81...25C ]
Hall, D.S. and Henry, G.W.: 1983, I.B.V.S. No. 2307.
Hartmann, L., Londono, C. and Phillips, M.J.: 1979, Astrophys.J.,
     229, 183. [BIBCODE 1979ApJ...229..183H ]
Henry, G.W.: 1983, I.B.V.S. No 2309.
Lines, R.D., Louth, H., Stelzer, H.J. and Hall, D.S.: 1983,
     I.B.V.S. No. 2308.
Nations, H.L. and Ramsey, L.W. : 1981, Astron.J., 86, 433. [BIBCODE 1981AJ.....86..433N ]
Rucinski, S.M.: 1977, Publ. Astron. Soc. Pac., 89, 280. [BIBCODE 1977PASP...89..280R ]
Zeilik, M., Elston, R., Henson, G., Schmolke, P. and Smith, P.:
     1982, I.B.V.S. No. 2177.