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IAUC 5684: 1992 QB1

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                                                  Circular No. 5684
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
Telephone 617-495-7244/7440/7444 (for emergency use only)
TWX 710-320-6842 ASTROGRAM CAM     EASYLINK 62794505
MARSDEN@CFA or GREEN@CFA (.SPAN, .BITNET or .HARVARD.EDU)


1992 QB1
     The following observations have been reported since the
October batch of Minor Planet Circulars was prepared (cf. IAUC 5633):

     1992 UT             R.A. (2000) Decl.         R    Observer
     Sept.24.37682   23 59 22.62   - 0 02 50.3          Rohde
          27.37038   23 59 08.96   - 0 04 17.0            "
     Oct. 26.42932   23 57 07.30   - 0 17 10.6          de Costa
          26.62049   23 57 06.59   - 0 17 15.9            "
     Nov. 15.15329   23 56 08.51   - 0 23 22.4          Monet
          16.16073   23 56 06.26   - 0 23 35.9            "
          23.05860   23 55 53.08   - 0 24 57.5   23.5   Storm
     Dec. 25.07396   23 55 47.23   - 0 25 18.4          Hainaut

J. R. Rohde, D. Pascu and A. K. B. Monet (U.S. Naval Observatory,
   Flagstaff Station).  1.55-m astrometric reflector + CCD.  Measurer
   J. A. DeYoung.
G. de Costa and K. Taylor (Anglo-Australian Observatory).  Measurer
   R. H. McNaught.
J. Storm, A. Smette and O. Hainaut (European Southern Observatory).
   3.5-m New Technology Telescope + EMMI.  Measurer Hainaut.

     The following improved orbital elements, by B. G. Marsden, satisfy
the 20 available observations Aug. 30-Dec. 25 with mean residual 0".45:

                    Epoch = 1993 Jan. 13.0 TT
     T = 2023 Aug. 10.4380 TT         Peri. =  46.3760
     e =  0.106879                    Node  = 359.4152  2000.0
     q = 39.641983 AU                 Incl. =   2.2221
       a = 44.385886 AU    n = 0.0033330    P = 295.7 years

The rather extreme precision is provided for the purpose of consistency,
not accuracy.  Considerable uncertainty should still be attached to most
of the elements.  It does seem, however, that the object is in a large,
low-inclination orbit and relatively close to its perihelion.  It is
quite likely that q is significantly smaller and e significantly
larger than shown above, but it is unlikely that the object could be
Neptune-crossing by more than a very small amount.


1992 December 30               (5684)              Brian G. Marsden

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