COMMISSION 27 OF THE I. A. U.
        INFORMATION BULLETIN ON VARIABLE STARS
                     NUMBER 385


                               Konkoly Observatory
                               Budapest
                               1969 October 4



             OBSERVATIONS OF AB COMAE

     At the Maria Mitchell Observatory about 50 plates
on a region in Coma Berenices have been obtained since 1964.
The star AB Com was rediscovered and examined relative to
nearby arbitrarily selected comparison stars by Janice
White. The star had originally been discovered by Hoffmeister
(S8491, 15m - 17m, A.N., 288, 49, 1964) who suspected it of
being a U Gem star, or possibly an RW Aur type. Miss White's
observations indicate maxima on JD 2438886 and 39256. The
star was not seen at a plate limit of about 16m on JD 38552,
40002-3, and 40348-382. These observations, combined with
the published date of Hoffmeister's maximum, JD 38501, and
its intermediate brightness on the Lick Atlas chart on
JD 35163 would not be inconsistent with a Mira type period
of 360 days. Further observations are needed.
      This note stems from part of the work carried out
by students at the Maria Mitchell Observatory under a grant
from the U. S. National Science Foundation.

September 24, 1969



                          DORRITT HOFFLEIT
                     Maria Mitchell Observatory
                      Nantucket, Mass, U. S. A.




                  BD +18deg4586

      This star is lettered K in the sequence for HR
(Nova) Delphini issued by the British Astronomical 
Association. The B.A.A. magnitude is given as 8.30; the B.D.
magnitude is 8.2; the spectrum is late-type, and the orange
colour is noticable in a small telescope.
      Having used the star as a comparison for HR Delphini,
I am now convinced that it is itself variable. The range
appears to be from 7.8 to 8.3, and the period may be semiregular 
(a few weeks?). I would however stress that these
results depend entirely upon visual observations with the
12 1/2 in. reflector in my observatory at Selsey, and will
certainly need to be confirmed by more accurate methods
before the variability of the star can be regarded as
established.

                         PATRIC MOORE
                         Farthings,
                         39 West Street
                         Selsey
                         Sussex, England





	             NOTE ON RU CAM


      During several months in spring and summer of 1968
the star was of irregular character. The star recovered its
periodic light variation in September, 1968 with an
amplitude of 0.1m in V. Later the amplitude decreased to
0.02m in V, having reached its minimum value in April and
May, 1969. Since then the amplitude was increasing and after
three cycles it reached the values 0.3m in V and 0.4m in B.



                          B. SZEIDL
                       Konkoly Observatory
                           Budapest