COMMISSION 27 OF THE I. A. U.
         INFORMATION BULLETIN ON VARIABLE STARS
                     Number 1698

                                    Konkoly Observatory
                                    Budapest
                                    1979 October 29



    ON THE VARIABILITY OF THE SUSPECTED BETA CEPHEI STARS
                V351, V356, V357 Per




     Hill (1967) has listed a number of suspected Beta Cephei
stars. Out of these the stars V351 Per (HD 13051), V356 Per
(BD 56d473) and V357 Per (HD 13866) were put on our observing
programme, in order to determine their variability.
     These stars were observed on a total of five nights 
between October 1978 to December 1978, on the 104-cm telescope of
the Uttar Pradesh State Observatory, Naini Tal, using EMI 6094S
photomultiplier tube cooled to -20dC and B filter of the Johnson
and Morgan system. The star HD 12994 was used as a comparison star.
The magnitudes were corrected for atmospheric extinction using
nightly extinction coefficients. The differential magnitudes
(Comparison-Variable) of V351, V356, V357 Per have been plotted
against J.D. (Hel.) in Figs. 1,2 and 3, respectively.
     From Figs. 1, 2 and 3 it is clear that none of the three
stars show any systematic variation. The B magnitude of these
stars are constant within +-0.01m which can be attributed to 
observational scatter. Therefore, we conclude that the stars
V351 Per, V356 Per and V357 Per are not Beta Cephei variables.





                              H. S. MAHRA and
                              VIJAY MOHAN

                              U.P. State Observatory,
                              Manora Peak,
                              Naini Tal - 263129
                              India

Reference:
Hill, G. 1967, Astrophys. J. Suppl. Ser. 14, 263 [BIBCODE 1967ApJS...14..263H ]


                             [FIGURE 1]

                  Fig. 1.  Light curves of V351 Per.

                             [FIGURE 2]

                  Fig. 2.  Light curves of V356 Per.

                             [FIGURE 3]

                  Fig. 3.  Light curves of V357 Per.