Central Bureau for Astronomical Telegrams
IAUC 4687: U Gem; V1333 Aql; VV Pup
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Read IAUC 4688
Circular No. 4687
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
U GEMINORUM
This object is again in outburst, as indicated by the
following visual magnitude estimates: Dec. 5.42 UT, 13.8 (G. Dyck,
North Dartmouth, MA); 5.94, 12.6 (G. Comello, Roden, The
Netherlands); 6.10, 9.8 (Dyck); 6.18, 10.0 (R. Hayes, Worth, IL);
6.20, 9.8 (Comello); 6.48, 9.3 (Hayes); 7.08, 9.4 (E. Mayer, Barberton,
OH); 7.18, 9.3 (Dyck); 7.18, 9.6 (L. Hiett, Arlington, VA); 7.21, 9.4
(Mayer). An alternative report gives the times of the Comello
observations as Dec. 5.7 and 6.25, respectively.
V1333 AQUILAE
S. A. Ilovaisky and C. Chevalier, Observatoire de Haute Provence,
communicate: "Analysis of a 1-min V-band image of the Aql X-1 transient
field obtained on Dec. 3.7 UT using the RCA3 CCD camera at the OHP 1.2-m
telescope reveals that one month after the Ginga x-ray detection (IAUC
4675) the optical counterpart V1333 Aql was still bright at V = 17.2,
approximately 2 mag above typical quiescent values as measured on CCD
images we obtained at ESO in 1986 Apr. with the 1.54-m Danish telescope
at La Silla and in 1988 May with EFOSC at the 3.6-m telescope".
VV PUPPIS
J. Bailey, Joint Astronomy Centre, Hawaii; and L. Ferrario and D.
Wickramasinghe, Australian National University, report:
"Spectropolarimetric observations of VV Pup made with the 3.9-m Anglo-
Australian Telescope on Nov. 29 and 30 show structure in intensity and
polarization which we identify with two sets of cyclotron harmonics.
One set is visible at all phases and shows peaks in intensity and
circular polarization at 660, 510, 420 and 350 nm, which can be modelled
as cyclotron radiation from a field of 57 MG. The other set is visible
only during the bright phase and shows peaks at 635, 550, 490 and 440
nm, corresponding to a field of 30 MG. The results can be understood in
terms of a dipole field distribution that is offset by 10 percent from
the center of the star, with the cyclotron emission occurring from two
regions slightly displaced from the magnetic poles. The field observed
for the secondary emission region is comparable with that in EXO
033319-2554.2, the highest known for an AM Her-type system (cf. IAUC
3340, 3380, 4517 and 4523)."
1988 December 7 (4687) Brian G. Marsden
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