COMMISSION 27 OF THE I. A. U.
        INFORMATION BULLETIN ON VARIABLE STARS
                    Number 1937

                                  Konkoly Observatory
                                  Budapest
                                  1981 March 17

                                  HU ISSN 0374-0676



        THE MAXIMUM TIMES AND NEW LIGHT ELEMENTS
                     OF kappa BOOTIS


During the intermediate and narrow band photometry of some Delta
Scuti type variables, kappa Boo was also observed at Ege University
Observatory with the 48 cm Cassegrain telescope on six nights in
June 1980 and twelve times of maxima were obtained. These times
of maxima are given in the following table. Since the period of
0.069d given by Millis (1966) does not agree with the new 
observations, the new period of 0.0762927d has been derived using
the times of maxima and the cycle numbers, and utilized.


                        Table

               The maximum times of kappa Boo



JD Hel.            O-C(I)         O-C(II)     E     Filter

2444 401.3670       0.0000d        0.0061d    1        b
        .3580    -   .0090     -    .0029     1        y
        .4435        .0002          .0063     2        b
        .4385        .0048          .0013     2        y

     404.3285    -   .0139     -    .0059     40       u
        .3290    -   .0134     -    .0054     40       v
        .3285    -   .0139     -    .0059     40       b
        .3315    -   .0109     -    .0029     40       y

     408.3770    -   .0089          .0018     93       v
        .3785    -   .0074          .0033     93       b
        .3800    -   .0054          .0048     93       y
 
     416.3035    -   .0169     -    .0009    197       y
                     
The O-C(I) residuals are the deviations from the light elements,

     Max.= JD Hel.2444 401.2907 + 0.0762927d E.
The least squares solution has been applied to these residuals
and cycle numbers(E), and the new light elements were derived as
follows,

     Max.= JD Hel.2444 401.2847 + 0.076242d E.
                           +-18       +-24

The O-C(II) residuals indicate the deviations from these new
light elements. The period we obtained is ten per cent longer
than that of Millis.
  The light curves and physical parameters of the star will
soon be published elsewhere.




                       S. EVREN, O. TUMER, Z. TUNCA,
                       A.Y. ERTAN., M. KURUTAC and
                       C. IBANOGLU

                       Ege University Observatory
                       Bornova, Izmir-TURKEY





Reference:
Millis, R.L. 1966, I.B.V.S. No. 137.