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IAUC 3377: 1979e; BD +66 1066 = NGC 6543

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IAUC number 

                                                  Circular No. 3377
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
TWX 710-320-6842 ASTROGRAM CAM     Telephone 617-864-5758


COMET TORRES (1979e)
     C. Torres, University of Chile, provides the following precise
positions, obtained at the Cerro El Roble Station:

     1979 UT             R. A. (1950) Decl.
     June 26.24860    19 49 27.24   -11 32 55.9
          28.24964    19 47 12.97   -11 16 06.8
          28.29790    19 47 09.56   -11 15 41.7
     July  2.20345    19 42 41.78   -10 42 58.4
           2.21734    19 42 40.41   -10 42 48.9

     The following parabolic orbital elements, by B. G. Marsden,
are necessarily somewhat uncertain (especially T and Peri.), but the
ephemeris should be satisfactory.

       T = 1979 Oct. 8.339 ET    Peri. =  21.99
                                 Node  = 292.46   1950.0
       q = 4.6060 AU             Incl. =  92.40

     1979 ET     R. A. (1950) Decl.     Delta     r      m1
     June 26    19 49.73    -11 34.8
     July  6    19 38.25    -10 11.2    3.682   4.667   17.6
          16    19 26.31    - 8 49.9
          26    19 14.51    - 7 32.9    3.674   4.644   17.6
     Aug.  5    19 03.43    - 6 21.7
          15    18 53.57    - 5 17.5    3.810   4.627   17.7

               m1 = 8.0 + 5 log Delta + 10 log r


BD +66 1066 = NGC 6543
     J. Patterson, University of Texas at Austin, writes: "Optical
photometry of the nucleus of this planetary nebula at the McDonald
Observatory reveals periodic oscillations in the lightcurve.  The
fundamental period is 47.73 s, but most of the power is at the
second harmonic (15.91 s).  The amplitude varies from 10 percent to
less than 0.4 percent on a timescale of a few hours.  Observations
are being continued to track the pulse phase.  Spectroscopic,
polarimetric and x-ray observations at high time resolution would be
of great interest.  The star is thought to be a binary system with
an 87-min orbital period (Lutz 1979, IAU Symp. No. 76)."


1979 July 9                    (3377)              Brian G. Marsden

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