COMMISSION 27 OF THE I. A. U.
               INFORMATION BULLETIN ON VARIABLE STARS
                            NUMBER 824

                        	       Konkoly Observatory
                               	       Budapest
                            	       1973 September 1


      OBSERVATIONS OF VARIABLES ON SKY PATROL PLATES



   GK And = Wr 170 was discovered by Weber and announced as an 
eclipsing binary (11.4m - 12.2m ph)(Weber, R. 1967, IBVS 183). Elements
of light variations were found by Kholopov (GCVS 1st Suppl. 1971). On
118 sky patrol plates (Sonneberg Obs. JD. 2439024 - 41602) I examined
the star and found 5 minima and improved elements:
   Min. (hel.) = JD. 2438643.430 + 2.009365d E      (EA)
           (11.28m - 12.36m/11.5m ph; D = 0.08p)

   EY Vul = GR 37 is a variable star discovered by Romano in 1958
(Oss. Treviso Publ. No.14). It is an eclipsing binary (11.2 - 12.0 ph).
I examined the star on sky patrol plates (Sonneberg Obs.) n = 374,
JD. 2435685 - 41602 (Hartha Obs.) n = 274, JD.2436810 - 41570 and found
the improved elements:
   Min. (hel.) = JD. 2435771.238 + 4.103052d E     (EA)
  (Max. = 11.16, Min.I = 12.19, Min.II = 11.21 ph, DI = 0.08p)

   HBV 489  This star was discovered in 1972 by Wachmann as an Algol-
type variable (11.80m - 12.63m ph). No elements were given(IBVS No.749).
Using 384 sky patrol plates (Sonneberg Obs.) I obtained the following 
elements:

   Min. (hel.) = JD. 2430633.378 + 4.980605d E        (EA)
          (12.02 - 12.8 ph; D = 0.04p)

   BD -5d2893  By observations of RU Sex I suspected the variability
of BD -5d2893. In order to test the variability I obtained 70 short-
exposures. There are irregular variations between 10.7m - 11.1m ph. The
star seems to be coloured.

VV 423 Miller discovered this variable star in 1971 and Wachmann,
(Hamburg Obs.) examined but could not find elements of this eclipsing
binary (Ric. astr. Specola Vatic. Vol. 8 No. 12). So I observed the star
on 472 sky patrol plates (Sonneberg Obs. JD. 2435695 - 41604). 12 minima 
and the following elements were obtained:

   Min. (hel.) = JD. 2433562.520 + 5.5337615d  E (EB)
             (Max. = 10.72m,    Min.I = 11.10m , Min.II = 11.76m ph)


CSV 8484 = GR 43 was discovered by Romano in 1958 (11.6m-12m ph).
220 plates of the sky patrol confirm the variability between the limits
11.50m - 12.33m ph. The type is presumable Isa.
Details for all these variables will be published in "Mitt. der Bruno-
H.-Burgel-Sternwarte Hartha" Heft 6.


     				                      H. BUSCH




       OBSERVATIONS OF 5 CSV - STARS ON SKY PATROL PLATES


   CSV 4548 = BD + 36d3414 (9.2) = SVS 868 = P 2486
I examined 140 plates of Hartha Observatory (JD. 2436817 - 38372). No
light variations were found.

   CSV 8390 = GR 32.  249 plates (JD. 2436810 - 41570) of Hartha Obs.
The period is about 0.5d, the type is RR Lyrae.
Observed maxima: JD.(hel.) 2436847.314, 2437129.379, 2437575.399,
2437886.446, 2437940.428, 2438351.304, 2438640.354, 2440483.341.
   CSV 8392 = GR 56. 136 plates of Sonneberg Observatory (JD. 2437559-
39792). The light variations are longperiodic.
   CSV 8474 = BD + 21d4117 = GR 54.   298 plates of Hartha Obs.
(JD. 2436810 - 41570). Unperiodical light variations were observed. The
star is not noticeable coloured. The type is presumably Isa.
   CSV 8518 = GR 52 = BD + 24d4131. 287 plates of Hartha Obs.
(JD. 2436810 - 41570). The star is probably a SRa-star with late
spectral type. I found a mean cycle of 362.5 days. The increasing lasts
20 - 40d. Mira-type is impossible because the amplitude is only 0.5m
(10.7 - 11.2m ph). Observed maxima: JD. 243 6825, 243 7195, 243 7947,
243 8284, 243 8664, 243 8995.
Further particulars and light curves will be given in "Mitt.der Bruno-
H.-Burgel-Sternwarte Hartha" Heft 6.





                          K. HAUSSLER