COMMISSION 27 OF THE I. A. U.
          INFORMATION BULLETIN ON VARIABLE STARS
                       Number 1059

                                    Konkoly Observatory
                                    Budapest
                                    1975 November 5



             NON-VARIABILITY OF NQ Her 



    Further to the observations of NQ Her in 1965 by Blanco (1),
in 1968 by Popovici (2) and Bozkurt, et al. (3) in 1972 the star
was observed by us photoelectrically on 11 nights during the five-
year interval May 1970 - May 1975. Our observations through U,B,V
filters (see Fig. 1) confirm these and earlier results of non-variability 
of the star at least since 1963. The plots in Fig. 1 are based on the 
ephemeris Pr.Min. = J.D. 2426894.433 + 0.870218d E mentioned 
by Kukarkin, et al. (4). BD + 18d3580 was used as a comparison
star. Considering the above behaviour of the star, it need no longer 
be considered a variable.





                         T.D. PADALIA
                  Uttar Pradesh State Observatory
                  Manora Peak, Nainital-263139, India.


References:

1) Blanco, C., 1971, I.B.V.S. No. 571
2) Popovici, C., 1971, I.B.V.S. No. 509
3) Bozkurt, S., Ibanoglu, C., Gulmen, O., Gudur, N., 1975,
        I.B.V.S. No. 1021
9) Kukarkin, B.V., Kholopov, P.N., Efremov, Yu.N., Kukarkina, N.P.,
   Kurochkin, N.E., Medvedeva, G.I., Perova, N.B., Pskovsky, Yu.P.,
   Fedorovich, V.P., Frolov, M.S., 1974, Second supplement
   to the third Edition of the General Catalogue of Variable Stars,
   Moscow.


                        [FIGURE 1]

  Fig. 1. Light curve of NQ Her
  The differential magnitudes are in the sense Variable minus Comparison.
  The +-2 sigma error bars for the Comparison Star are indicated along 
  the side.