COMMISSION 27 OF THE I. A. U.
         INFORMATION BULLETIN ON VARIABLE STARS
                     Number 2051

                                 Konkoly Observatory
                                 Budapest
                                 1981 December 4

                                 HU ISSN 0374-0676





           SPECTROSCOPY OF V1425 CYGNI AND AH CEPHEI


      The star HD 202000 was discovered to be variable by the
Bamberg Observatory and was given the provisional designation
BV 346. Its HD spectral type is B8, and the visual magnitude of
the system is 7.7 at maximum light. Photoelectric light curves of
this eclipsing binary were obtained by Tate (IBVS Nr. 438), who
also determined its period to be 1.252387 days. Subsequently
the star was named V1425 Cygni.
      On October 7 through 11, 1981, this investigator obtained
seven spectrograms of V1425 Cygni using the 1.0 meter coude feed
telescope of the Kitt Peak National Observatory. The emulsion used
was IIaO, and the dispersion was 16.9 A/mm. It was hoped that the
system would prove to be a double-lined spectroscopic binary, since
the two minima are approximately of the same depth. The Balmer
lines, however, are extremely broad and are hopelessly blended at
all orbital phases, and the weaker lines are all washed out by
rotation. Interstellar H and K lines were present, and for the
K line a mean velocity of -20 +- 2 km/s was obtained. The diffuse
interstellar absorption feature at 4430 was not observed.   
      The eclipsing binary AH Cephei was also observed on four
nights between October 7 and 11, 1981. The spectral type of this
star is B1, and the lines are diffuse and strongly broadened by
rotation. The interstellar H and K lines of CaII are very strong
and show a radial velocity of -31 +- 1 km/s. This value can be
compared with the gamma-velocity for this system of -20.6 km/s
obtained by Harper et al. [J. R. A. S. Canada, vol. 29, 413, 1935).
The measurements used in determining the orbit which was reported
in that paper showed a high degree of scatter, and it was hoped
by this investigator that the orbit could be improved, but all
of the spectral lines of AH Cephei proved to be extremely broad
and shallow.
     This investigator wishes to acknowledge the support which
he received from a Small Research Grant from the American 
Astronomical Society.





              C.R. CHAMBLISS
              Dept. of Physical Sciences
              Kutztown State College
              Kutztown PA 19530
              USA