COMMISSION 27 OF THE I. A. U.
            INFORMATION BULLETIN ON VARIABLE STARS
                            NUMBER 40

                                           Konkoly Observatory
                                           Budapest
                                           20 November 1963


                 PHOTOELECTRIC AND SPECTROSCOPIC
              OBSERVATIONS OF 48 PERSEI AND 53 PERSEI


     The Be-star 48 Persei has already been observed some time
ago (see VSS 5, No. 5). In order to get acquainted more accurately with
the light variation the star was observed photoelectrically in February
and March 1963 in the yellow region. During this time it had a maximum
as well as a minimum of brightness; the amplitude is 0m.10. In case
the light variation should be periodic which is probable, at least
approximately, the "period" during the time of observation might be
about 55 days.
      The spectrum of this star was taken simultaneously on Agfa-Z
emulsion. The plates show the Balmer series beginning with H_gamma. H_gamma,
H_delta and H_epsilon are often to be seen with emission components. A certain
frequency of the emissions might be possible during the descent
towards the minimum of brightness, the emissions showing then
sometimes central absorptions.

      Together with 48 Persei the star 53 Persei has been observed
photoelectrically in V. Its brightness fluctuates within about 0m.15.
Even if one takes into consideration that the error of the measurements
is larger in this case than with 48 Per, yet the range of 0m.07 must be
regarded as absolutely certain. A period could not be determined.

      Details of both stars will soon be published in MVS.


                                            G. JACKISCH
                                       Sonneberg Observatory