COMMISSION 27 OF THE I. A. U.
        INFORMATION BULLETIN ON VARIABLE STARS
                     NUMBER 502
                       			Konkoly Observatory
                       			Budapest
                       			1970 December 31

        PHOTOELECTRIC LIGHT-CURVE OF KP Aql

      The eclipsing binary KP Aql (BD+15d3667) was 
observed photoelectrically between August 1 and October 9,
1970 on eleven nights with the 48 cm Cassegrain telescope
of the Ege University Observatory. An RCA 1P21 
photomultiplier and the filters Corning No. 5030 + Schott GG 13 for
B and Corning No. 3384 for V were used.
      The have obtained between 1988 August and 1970 October 
5 minima. They all show very large O-C's against the
elements C_I given in GCVS (1969) (s. Table I, O-C_I) 
Calculations of new light-elements were made from 15 minima.
The weighted least square solution gives the following new
elements:

      Hel. Min = JD 2 436 712.4685+1.6837392d.E (C_II)
                              +-25      +-13   (m.e)

Table I. shows the observed times of the minima, the values
of O-C_I and O-C_II, their weights (p) and references to 
observers, (Gl.= Omur Gulmen, Ib = Cafer Ibanoglu, Kt= Mehmet
Kurutac).



                   Table I

            O           O-C_I   O-C_II  p    Obs

     2433858.549 v    +0.001  +0.018    1    AN 281
       34910.859 pg   -0.018  -0.009    2    AJ 66
       35333.485 v    -0.008  -0.001    1    AN 286
       35355.364 "    -0.017  -0.011    1    "
       36025.507 "    +0.003  +0.004    1    "
       36106.331 "    +0.008  +0.009    1    "
       36451.502 "    +0.015  +0.013    1    "
       36712.465 n     0.000  -0.004    1    "
       37921.377 "    -0.004  -0.016    1    AN 288
       37948.322 "    +0.001  -0.011    1    "
       40098.471 pe   +0.031  +0.003    3    Ib/Kt
       40396.4914 "   +0.0317 +0.0015   5    Ib/Gl
       40822.477  "V  +0.034  +0.001    3    Ib/Gl
       40839.3129 "V  +0.0330 -0.0004   5    Ib/Gl
       40866.2529 "V  +0.0331 -0.0005   5    Ib/Gl


The light-curves are shown in Figures I and II where
the magnitude differences between the variable and the
comparison star BD+15d366 have been plotted against phase
using the new elements. The star varies about 0.70m in both
yellow and blue. Both light-curves are similar with some
exception in the phase-interval 0.825p-0.925p, We have 
observed some anomalous effect in this interval in V on August
1 and 2, 1970.
We are planning to obtain further observations to
fill the phase-interval 0.275p to 0.400p, and to re-examine
the unexpected behaviour between 0.825p and 0.925p. We hope
to clarify these points in the coming observing season.


                    CAFER IBANOGLU, OMUR GULMEN
                    Ege University Observatory
                           P.K. 21
                      Bornova-Izmir, TURKEY


                      [FIGURE 1]
                      [FIGURE 2]