COMMISSION 27 OF THE I. A. U.
            INFORMATION BULLETIN ON VARIABLE STARS
                         Number 3400

                                          Konkoly Observatory
                                          Budapest
                                          5 December 1989

                                          HU ISSN 0374 - 0676


              PHOTOMETRY OF SUSPECTED UU Her-STARS


Some years ago Sasselov (1984) published a list of suspected UU Her variables
based on the spectral classification of Bartaya (1979). Some of these stars
were included in a program to determine if they were really variable. A
similar work was carried out by Arellano Ferro et al. (1989), who concluded
that most of the stars in this list were not supergiants, i.e. do not belong
to the UU Her-class.

The photometric observations were carried out in Piszkesteto with the 50-cm
telescope of Konkoly Observatory in the UBV system during 1985-1988. The stars
were not observed systematically, mainly because of the usual unfavourable
spring weather. Table I contains the results of the observations.

TABLE I

star        comparison   number of     DeltaV     Delta(B-V)     Delta(U-B)
                       observations
HD 51832    HD 50864     4          -0.734+-0.009 -0.037+-0.003 +0.157+-0.007
HD 56664    BD +61d 968  2          +0.746+-0.006 +0.071+-0.004 +0.035+-0.001
HD 58965    HD 59506     6          +1.258+-0.017 -0.650+-0.005 -0.972+-0.009
HD 58966    HD 59506     6          +0.873+-0.004 -0.665+-0.009 -0.984+-0.004
HD 102102   HD 101549    4          +0.117+-0.002 +0.152+-0.004 +0.008+-0.012
HD 102570   HD 102482    4          -0.313+-0.006 -0.539+-0.004 -0.598+-0.012
HD 130667   BD +47d 2178 6          -0.967+-0.007 -0.091+-0.005 +0.066+-0.012

It is clear that these stars are not variables. HD 58965 may be the only
exception, but if the larger scatter is due to variability, it probably is not
of the UU Her-type (the amplitude is smaller than 0.05 mag). There are only
two measurements of HD 56664 with differences of 0.008 mag in V, 0.005 mag in
B-V and 0.001 in U-B, but there is a three year long gap between them. Thus
the UBV photometry of these stars supports the conclusion of Arellano Ferro et
al. (1989) that these stars are definitely not UU Her-type variables.


E. ZSOLDOS
Konkoly Observatory
Budapest XII. P.O. Box 67
1525 HUNGARY

References

Arellano Ferro, A., Giridhar, S., Chavez, M., Parrao, L. 1989, A.Ap. 214, 123 [BIBCODE 1989A&A...214..123A ]
Bartaya, R.A. 1979, Abastumani Bull. No. 51, p. 1 [BIBCODE 1979AbaOB..51....1B ]
Sasselov, D. 1984, Ap. Space Sci. 102, 161 [BIBCODE 1984Ap&SS.102..161S ]