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IAUC 3730: 1982g; CPD -48 1577

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IAUC number 

                                                  Circular No. 3730
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 AUSTIN (1982g)
     The following elliptical orbital elements are from MPC 7230.
Perturbations by all nine planets were taken into account.

                   Epoch 1982 Aug. 19.0 ET
         T = 1982 Aug. 24.7269 ET  Peri. =  33.8229
         e =   0.999600            Node  = 325.5646   1950.0
         q =   0.647797 AU         Incl. =  84.4917

     1982/83 ET R.A. (1950.0)  Decl.      p        r       m1

     Sept.28    12 51.03    +37 55.2    1.464    0.956     8.6
     Oct.  8    12 55.70    +35 57.7
          18    12 59.43    +34 28.3    1.755    1.252    10.2
          28    13 02.34    +33 27.7
     Nov.  7    13 04.22    +32 55.7    1.901    1.553    11.3
          17    13 04.72    +32 52.8
          27    13 03.32    +33 19.7    1.937    1.846    12.1
     Dec.  7    12 59.41    +34 16.2
          17    12 52.23    +35 41.3    1.904    2.129    12.7
          27    12 40.88    +37 30.8
     Jan.  6    12 24.57    +39 35.4    1.861    2.402    13.2
          16    12 02.78    +41 39.8
          26    11 35.91    +43 23.3    1.885    2.666    13.6
     Feb.  5    11 05.74    +44 25.4
          15    10 35.17    +44 34.6    2.042    2.921    14.2
          25    10 07.35    +43 52.9
     Mar.  7     9 44.37    +42 33.3    2.352    3.168    14.9


CPD -48 1577
     R. F. Garrison, David Dunlap Observatory: W. A. Hiltner,
University of Michigan: and R. E. Schild, Center for Astrophysics,
write: "The star CPD -48 1577 has been found to have a spectrum
characteristic of the cataclysmic variables, and at V = 9.8 it
would be the brightest known such object.  It has colors similar
to those of UX UMa and flickering brightness fluctuations of order
0.1 mag on a timescale of minutes.  Larger variations were found
on a timescale of years.  The extremely broad, shallow H absorption
lines have emission cores with a very slow Balmer decrement.
Extremely weak, broad absorption lines of He I and He II are probably
present."


1982 October 8                 (3730)              Brian G. Marsden

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