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IAUC 5505: 1992g; HV Vir

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                                                  Circular No. 5505
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)


PERIODIC COMET MUELLER 4 (1992g)
     S. Nakano, Sumoto, Japan, communicates further precise positions
by T. Seki, Geisei, and an improved orbit from observations Apr. 9-22:

     1992 UT             R.A. (2000) Decl.        m1
     Apr. 20.52257   14 07 11.99   +29 23 21.6   17.5
          20.54167   14 07 11.45   +29 23 26.5
          22.56076   14 06 04.23   +29 35 20.0   18

     T = 1992 Feb. 15.135 TT          Peri. =  43.287
     e = 0.38878                      Node  = 145.613   2000.0
     q = 2.65571 AU                   Incl. =  29.976
       a =  4.34493 AU     n = 0.108825     P =   9.06 years

1992 TT     R. A. (2000) Decl.     Delta      r    Elong. Phase      m1
Apr. 28    14 03.09    +29 59.6    1.886    2.698  135.6   15.1     17.2
May   8    13 58.13    +30 15.3    1.947    2.711  130.2   16.5     17.3
     18    13 54.46    +29 55.8    2.023    2.724  124.3   17.9     17.4
     28    13 52.54    +29 06.1    2.112    2.739  118.1   19.1     17.5
June  7    13 52.60    +27 51.5    2.212    2.756  111.8   20.0     17.6
     17    13 54.70    +26 18.1    2.321    2.774  105.7   20.6     17.8
     27    13 58.71    +24 30.9    2.436    2.793   99.7   21.0     17.9


HV VIRGINIS
     S. Howell, Planetary Sciences Institute; R. M. Wagner and R.
Bertram, Ohio State University; and P. Szkody, University of
Washington, report: "A spectrum (range 430-710 nm, resolution 1 nm)
obtained on Apr. 23.17 UT with the Perkins 1.8-m telescope at the
Lowell Observatory shows broad Balmer and He I absorption lines, but
with weaker emission cores than reported one night earlier (IAUC
5503).  He II 468.6 nm was weak or absent.  This observation confirms
that HV Vir is a dwarf nova and not a classical nova as was originally
thought.  Preoutburst measurements obtained in Mar. and Apr. 1989 gave
V = 19.10, B-V = +0.26, V-R = -0.07, V-J = +1.9 (the V-J color being
obtained one month apart).  The high galactic latitude and 8-mag
outburst amplitude of this star make it similar to other high
latitude, large-outburst amplitude dwarf novae discussed by Howell and
Szkody (1990, Ap.J. 356, 623)."


1992 April 25                  (5505)              Brian G. Marsden

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