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IAUC 5360: 1991y; V1017 Sgr

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IAUC number 

                                                  Circular No. 5360
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


PERIODIC COMET McNAUGHT-HUGHES (1991y)
     R. H. McNaught provides the following additional measurements
from films taken with the Uppsala Southern Schmidt telescope at
Siding Spring:

     1991 UT             R.A. (1950) Decl.
     Oct.  2.55556   23 09 09.64   -18 47 58.9
           2.73611   23 09 05.38   -18 47 46.3
           5.52552   23 08 06.55   -18 44 11.9

     The following preliminary orbital elements, from the six
available observations, indicate that this is a short-period comet:

     T = 1991 June 29.248 ET          Peri. = 231.290
     e = 0.39604                      Node  =  87.864   1950.0
     q = 2.17255 AU                   Incl. =   7.304
       a =  3.59718 AU     n = 0.144464     P =   6.82 years

     1991 ET      R.A. (1950) Decl.     Delta      r       m1
     Oct.  1    23 09.79    -18 49.1    1.345    2.277    16.5
           6    23 07.96    -18 43.4
          11    23 06.70    -18 31.9    1.427    2.299    16.7
          16    23 06.05    -18 15.0
          21    23 06.04    -17 53.0    1.527    2.323    16.9
          26    23 06.66    -17 26.5
          31    23 07.90    -16 55.9    1.642    2.349    17.1


V1017 SAGITTARII
     K. Sekiguchi, South African Astronomical Observatory; and D. W.
Latham, Center for Astrophysics, report:   "Spectra of V1017 Sgr
obtained Aug. 6-13 at SAAO, Sutherland, are similar to 1990 spectra
when the star was at minimum.  By Sept. 10-17, the spectra showed a
strengthened blue continuum.  Spectra obtained Oct. 2-4 show a blue
continuum and narrow (FWZI about 700 km/s) Balmer emission lines, He
I and II, and a weak 464.0-nm blend, with He II 468.6-nm the strongest
line.  The observed features are similar to those seen in 1973
(Vidal and Rodgers 1974, PASP 86, 26) and are consistent with a
brightened accretion disk (cf. Webbink et al. 1987, Ap.J. 314, 653)."


1991 October 7                 (5360)             Daniel W. E. Green

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