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IAUC 5098: 1990 SB; 1990c

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IAUC number 

                                                  Circular No. 5098
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 or GREEN@CFA.BITNET    MARSDEN or GREEN@CFAPS2.SPAN


1990 SB
     H. E. Holt and J. A. Brown report their discovery of a
fast-moving asteroidal object on Palomar 0.46-m Schmidt telescope
films exposed by them, H. R. Holt, and C. M. Olmstead.
Measurements by E. Bowell:

     1990 UT             R.A. (1950) Decl.       Mag.
     Sept.16.47205    1 38 37.65   +12 01 54.7   16.0
          16.50451    1 38 35.55   +12 01 05.7
          18.42344    1 36 40.52   +11 13 02.4   15.8
          18.45625    1 36 38.40   +11 12 10.8
          20.40602    1 34 35.39   +10 22 59.4   16.0
          20.48281    1 34 30.10   +10 21 02.7

     Orbital elements by Bowell from the above observations:

     T = 1990 May  23.835 ET          Peri. =  86.958
     e = 0.56042                      Node  = 189.892   1950.0
     q = 1.07805 AU                   Incl. =  18.005
       a =  2.45245 AU     n = 0.256627     P =   3.84 years

     1990 ET      R.A. (1950) Decl.     Delta      r       V
     Sept.16     1 39.09    +12 13.8
          26     1 28.29    + 8 01.7    0.791    1.763    15.1
     Oct.  6     1 16.45    + 4 00.5
          16     1 05.49    + 0 33.5    0.919    1.910    15.3


COMET LEVY (1990c)
     S. Larson and D. Levy, University of Arizona, communicate:
"On Sept. 17.1 UT, we obtained Cousins red-band CCD images of
comet 1990c with the Catalina 1.5-m telescope that showed (after
spatial filtering) two well defined hoods, 12 300 and 22 200 km
sunward from the nucleus and extending from p.a. 190 to 10 degrees
(the sunward hemisphere), symmetric with respect to the heliocentric
vector.  We saw no change during the short observing window, and
spectra indicate that they are most likely dust.  It would be very
useful if observers could obtain images to see how fast they change
and if they correlate with the photometric variations reported by
Schleicher et al. (IAUC 5081)."


1990 September 22              (5098)             Daniel W. E. Green

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