COMMISSION 27 OF THE I. A. U.
         INFORMATION BULLETIN ON VARIABLE STARS
                     Number 2388

                                     Konkoly Observatory
                                     Budapest
                                     19 August 1983

                                     HU ISSN 0374-0676


            OPTICAL BEHAVIOR OF EZ PEGASI



   The unique variable EZ Pegasi at position alpha = 23h14m26s
delta= 25d26.8' (1950), and of spectrum G5 (General Catalogue of
Variable Stars, 3rd Ed.), underwent a flare in November 1943
when its G5 spectrum was observed to have changed to B
(Vyssotsky and Balz 1958). Examination of Harvard Observatory
photographic plates by G. Mumford showed irregular variation
from magnitude 9.5 to 10.5 (Alden 1958).
Spectroscopic observations by Irvine between October 1971
and January 1972 showed normal G5 V spectra in the blue except
for Hbeta that appeared as a "very broad, weak absorption with
possible core emission." Spectra in the visual region revealed
short-term fluctuations in the intensity of Halpha emission (Irvine
1972). Irvine concluded that the 1943 B spectrum represented a
flare, and as the star lacks characteristics of an ordinary
flare star, he suggested it to be a probable U Geminorum-type
system.
  As a result of recent requests to the American Association
of Variable Star Observers (AAVSO) from several astronomers
concerning the behavior of EZ Peg, the long-term AAVSO
observations of this star were compiled. Figure 1 is an AAVSO
finder chart and Figure 2 is the AAVSO visual light curve
composed of individual observations of EZ Peg. The visual
light curve shows an apparent constant brightness at 9.6 +-0.2
magnitudes. Analysis of 30-day means of these observations did
not show conclusive evidence of periodic variation. Also, a
survey of the long-term observations of individual observers
confirmed the constancy of its light behavior.

                      [FIGURE 1]

   Figure 1  AAVSO finder chart of EZ Peg. The variable W Peg
   also appears on the chart,

                      [FIGURE 2]

   Figure 2  AAVSO visual light curve from 1972 to 1982. Each point
   represents one observation.

  Continued optical monitoring along with spectroscopic
observations are needed to further determine the nature of this
interesting star. The author wishes to acknowledge the
contribution of the observers of the AAVSO.


   SHELLY K. POPE
   American Association of Variable Star Observers (AAVSO)
   187 Concord Avenue
   Cambridge, Massachusetts 02138
   U.S.A.





References:

Alden, H. L. 1958, Astrophys. Journ 63, 358. [BIBCODE 1958AJ.....63..358A ]
Irvine, N. J. 1972, Publ, Astron, Soc. Pacific 84, 671. [BIBCODE 1972PASP...84..671I ]
Vyssotsky, A. N. and Balz, A. G. A. 1958, Publ. Leander
   McCormick Obs, 13, II, 79.