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IAUC 7343: C/1998 G3, C/1999 Y2; QY Per; V1494 Aql

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IAUC number

                                                  Circular No. 7343
Central Bureau for Astronomical Telegrams
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
URL http://cfa-www.harvard.edu/iau/cbat.html  ISSN 0081-0304
Phone 617-495-7244/7440/7444 (for emergency use only)

COMETS C/1998 G3 AND C/1999 Y2
     K. Cernis, Vilnius, Lithuania, reports his discovery of an
apparent comet (discovery position below) at mag about 5 on SOHO
images taken on 1999 Dec. 28 that were posted on the SOHO website.
D. A. Biesecker, SM&A Corporation and Goddard Space Flight Center,
reports that the comet was visible on both LASCO C2 and C3 images
and that no tail was detected.  Astrometric measurments by
Biesecker and D. Hammer (University of Maryland), reduced by
Marsden, appear on MPEC 2000-A36, together with parabolic orbital
elements (q = 0.048 AU, i = 111.4 deg), showing that the comet is
not a Kreutz sungrazer.  Magnitude reductions by Biesecker and
Hammer show that the comet faded from mag 6.1 to 6.8 during Dec.
28.58-28.79, and thence from view while still in the C3 field.

     1999 UT            R.A. (2000) Decl.
     Dec. 28.279      18 28.3       -26 10

     New astrometric measurements and orbital elements for C/1998
G3 (cf. IAUC 6952) appear on MPEC 2000-A37.  This comet is also
not a Kreutz sungrazer.

     T. Kato, Kyoto University, reports on behalf of the VSNET QY
Per collaboration team:  ''Unfiltered CCD photometry of QY Per has
been undertaken since 1999 Dec. 29.356 UT by numerous observers
around the world (T. Kato, M. Uemura, K. Matsumoto, G. Masi, A.
Cassetti, L. Cook, L. T. Jensen, B. Martin, T. Vanmunster, and D.
Buczynski).  Analysis of the combined light curve (covering 8 days)
revealed the clear existence of superhumps, with an average period
of 0.07861 day, including the prominent growth of superhumps
starting around Dec. 29.7.  The fairly long outburst interval and
the long superhump period suggest that QY Per does indeed belong
(cf. IAUC 7340) to a relatively rare class of long-period SU UMa-
type dwarf novae.  The light curve can be seen at

     Visual magnitude estimates:  1999 Dec. 26.699 UT, 7.7 (R. J.
Bouma, Groningen, The Netherlands); 29.727, 7.6 (Bouma); 2000 Jan.
3.714, 8.1 (S. Baroni, Milan, Italy); 5.702, 8.0 (K. Hornoch,
Lelekovice, Czech Republic).

                      (C) Copyright 2000 CBAT
2000 January 10                (7343)            Daniel W. E. Green

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