Commission 27 of the I. A. U.
        Information Bulletin on Variable Stars
                       Number 7


                                 Konkoly Observatory
                                 Budapest
                                 19 March 1962

               NEW BRIGHT VARIABLE STAR

      According to our photoelectric observations the
star BD + 40deg 4502 (= PD 12356 = HD 203712 = No 102090
in Moscow Catalogue of Stars Suspected of Variability)
appears to be a semiregular or irregular variable.
Spectral type : gM6(WILSON), brightness : 7^m,24 (HR). The
comparison star used was BD+ 40deg 4503, B5, 7^m,42 (HR).
The visual brightness of the variable declined from 7^m,53
on October 11, 1961 to 7^m,87 on October 31, and thereafter
increased with marked fluctuations to 7^m,49 on December
18, 1961. On November 15, 1960 the brightness of the
variable was 7^m,42. The star was suspected of variability
already by PICKERING (HA 45) and by MULLER and KEMPF
(Potsdam Publ. 17).

                                   H. v. SOCHER
                             Universitats-Sternwarte
                                     Wien




                     SZ LYNCIS

      This bright variable (BD + 44deg 1718, 8^m,8) was 
recently shown by SCHNELLER (AN 286, 102.1961) to be an
RR Lyrae-star belonging to the short-period group. In
February and March, 1962 about 600 observations were 
obtained in blue and yellow colours with a photoelectric
photometer coupled to our 24-inch reflecting telescope.
These observations, combined with Schneller's epochs,
provide the ephemeris:
  Max.helio. = J.D. 2437718,5568 + 0^d,12053487. E.
The light-range is 0^m,67 in blue and 0^m,54 in yellow. No
beat-phenomenon is apparent in the light-variations of
the star; but the light-curve shows minor deviations
from epoch to epoch.
                          K. GEFFERTH and B. SZEIDL
                             Konkoly Observatory
                                  Budapest





                  THE PERIOD OF SZ LYNCIS

      Using SCHNELLER's photoelectric observations
(AN 286,102,1961) and the epochs of maxima and minima
published by SOLOVIEV (Astr. Circ. USSR 159,17) and
ZESSEVITCH (Astr. Circ. USSR 170,16) the following formula
was obtained for times of maximum light:
  Max = 2437368,403 + 0^d,12053473. E, P^{-1} = 8,29636404
The epochs of minima given by Zessevitch were transformed 
to epochs of maxima by addition of a correction
+O^d,050 (to the visual minima a correction +0^d,045 was
applied).
      The residuals corresponding to the formula
above, listed under the heading O - C, are, in general
large owing to the low accuracy of the epochs.

   Maxima              O - C         Maxima          O - C
2433357,26     S     +0^d,012     2434414,20   S    -0^d,017
   3392,20     S     -0,003          4440,359  Z    -0,014
   3946,549    Z     +0,006          4445,21   S    +0,015
   3947,607    Z     -0,020          5592,339  Z vis+0,015
   4034,18     S     +0,009          5593,392  Z  " -0,017
   4041,522    Z     -0,002          7368,403 Sch pe.0,000
   4064,437    Z     +0,011

   S = Soloviev,    Z = Zessevitch,    Sch = Schneller



                                    P. NOTNI
                                   Sternwarte
                                   Babelsberg