COMMISSION 27 OF THE I. A. U.
          INFORMATION BULLETIN ON VARIABLE STARS
                      Number 1566

                                  Konkoly Observatory
                                  Budapest
                                  1979 March 9




IS THE NEW, VERY RED VARIABLE, THE COMPANION IN THE SOUTH-SOUTH-WEST
DIRECTION TO THE SUSPECTED VARIABLE BD+51d762 A MOST REMARKABLE STAR ?


Some months ago I got acquainted with the star BD+51d762 suppossed 
to be a red variable. I observed the star on more than 350
photographic plates of the Harvard College Observatory Collection
and a few photovisual plates. Almost at once the star was a 
disappointment. But then, persisting and curious still I was rewarded
second to none: I found another star - the companion to BD +51d762
which fulfilled two most important prerogatives for the variable
stars - a distinct variability of brightness and its periodicity
or at least an obvious cyclicity. Moreover, the star showed  not
one variation but three. A unique phenomenon among the red variables 
of any kind. I write them:

---------------------------------------------------------------
Duration           Amplitude of variation   Period or Cycle
                                            (not irregular!)
---------------------------------------------------------------
Longest            10.98m - 12.04m          5300days +- 250 days
Medium             10.95  - 12.00             475"   +-   35"
Short              10.85  - 11.35                 0.26 day
---------------------------------------------------------------

There is only one out of some 500 N Sp. Variables which has two
definite variations of brightness, with two corresponding periods:
2450 and 212 days. It is important though the Creator may smile
at it that their mutual ratios are almost identical 11.2 and 11.5.
This with the triplet variation suggesting three body problem only
accentuets the possibility that this new N or Carbon Variable
belongs to the 42 Most Remarkable Stars established during the
Golden Age of Stars i.e. between 1920 and 1953.
The magnitudes are approximately on the International system with
the Zero point obviously more uncertain than the Scale. The Palomar-
Mine Color Index is ~ 5 mg!



                                            SERGEI GAPOSHKIN
                                            Harvard College Observatory
                                            Cambridge, Ma., 02138,
                                            U.S.A.