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IAUC 4722: DX And; 1985 DO2 AND (3908); 1987 VII; NSV 01098

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IAUC number 

                                                  Circular No. 4722
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


DX ANDROMEDAE
     This cataclysmic variable star with infrequent eruption is
undergoing an outburst, as indicated by the following visual magnitude
estimates: Jan. 20.96 UT, [13.6 (G. Dyck, North Dartmouth, MA); 21.97,
13.1 (Dyck); 22.96, 12.8 (Dyck); 24.76, 11.8 (P. Schmeer, Bischmisheim,
West Germany); 24.78, 11.7 (Schmeer); 24.97, 11.5 (Dyck).  J. Mattei,
who communicated the Dyck observations, adds that the previous recorded
outbursts in AAVSO data files have been in 1988 Jan., 1987 May (cf. IAUC
4387), 1986 May, 1985 July and 1984 July.  High-speed photometry during
this outburst is recommended.


1985 DO2 AND (3908) 1980 PA
     J. Luu, Massachusetts Institute of Technology; and D. Jewitt,
University of Hawaii, report: "Optical CCD spectra taken in 1988 Sept.
(2.4-m telescope, McGraw-Hill Observatory) and Oct. (2.1-m telescope,
Kitt Peak National Observatory) show weak but definite features at 430,
505 and 550 nm in the near-earth minor planets 1985 DO2 and (3908) 1980
PA.  These features are identified as spin-forbidden absorptions due to
Fe++ in pyroxene.  To our knowledge, none of these absorptions has been
previously detected in the spectrum of any minor planet."


COMET WILSON (1987 VII)
     S. Larson and D. Levy, Lunar and Planetary Laboratory, communicate:
"Broadband red CCD images with the Catalina 1.5-m reflector on Jan.
11.326 UT show the secondary nuclear condensation separated from the
primary by 30".5 in p.a. 125.5 deg (cf. IAUC 4552, 4555, 4557).  The
secondary is about two magnitudes fainter than the primary and appears
somewhat extended.  Z. Sekanina, Jet Propulsion Laboratory, indicates
that a least-squares fit to 12 observations between 1987 Dec. and 1989
Jan. yields a time of splitting of 1987 Sept. 11 +/- 5, a relative
nongravitational deceleration of 69 +/- 4 units of 10**-5 solar
attraction and a separation velocity of 4.0 +/- 0.1 m/s, mostly in the
orbit plane."


NSV 01098
     Visual magnitudes: Jan. 13.89 UT, 10.1 (A. Pereira,
Linda-a-Velha, Portugal); 14.03, 9.7 (P. Schmeer, Bischmisheim, W.
Germany); 14.87, 10.1 (Pereira); 19.98, 10.1 (Pereira); 22.95, 10.0
(Pereira); 24.88, 9.9 (Schmeer).


1989 January 25                (4722)              Brian G. Marsden

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