Central Bureau for Astronomical Telegrams
IAUC 2994: NOVALIKE OBJECT IN Oph; X-RAY BURSTS; 1976e; 1975j; AM Her
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Read IAUC 2995
Circular No. 2994
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
Cable Address: SATELLITES, NEWYORK
Western Union: RAPID SATELLITE CAMBMASS
NOVALIKE OBJECT IN OPHIUCHUS
K. Osawa, Tokyo Astronomical Observatory, cables that V.
Kuwano, Hita, Oita, has discovered a novalike object as follows:
1976 UT R. A. (1950) Decl. mpv
Sept.23.55347 18 00.9 +11 48 8.8
Other magnitude estimates: Sept. 24.52 UT, mpv = 8.8; 28.49, mv =
10.5. The object was evidently fainter than magnitude 10 from May
until as recently as Sept. 17.48 UT.
X-RAY BURSTS
W. H. G. Lewin, J. A. Hoffman and J. Doty, Massachusetts
Institute of Technology, report the discovery by SAS 3 of x-ray
bursts from MXB1659-29 at R.A. = 16h59m.0, Decl. = -29o52' (equinox 1950.0).
The error ellipse has semiaxes 5' and 4' the major axis being in
p.a. 110o-290o. Between Oct. 2 and 9, 24 bursts (typically of
30s duration) were observed, the burst intervals changing from ~
2h.2 to ~ 2h.6 during the observations. The peak burst intensity was
about one-third that of the Crab (at 1-12 keV). The nearby globular
cluster NGC 6266 is definitely excluded as the source of the
bursts, and a careful search by W. Liller, Center for Astrophysics,
of the Palomar Sky Survey prints revealed no obvious optical
candidate. During the same observing period, 16 bursts were observed
from MXB1728-34 (burst intervals ~ 7h.8); no bursts were observed
from the rapid burster MXB1730-335.
PERIODIC COMET D'ARREST (1976e)
Further precise positions have been reported as follows:
1976 UT R. A. (1950) Decl. m1 Observer
July 30.91460 20 22 12.35 + 8 49 07.8 11 Benisek
Aug. 5.85938 20 54 12.22 + 0 33 18.4 Hers
5.86632 20 54 14.46 + 0 32 38.6 "
6.88021 21 00 20.13 - 1 05 23.5 "
6.91493 21 00 32.01 - 1 08 47.1 "
11.73958 21 31 47.40 - 9 29 24.2 "
11.74653 21 31 50.20 - 9 30 07.8 "
12.78542 21 38 55,43 -11 21 18.3 "
12.78958 21 38 57.04 -11 21 44.4 "
13.86458 21 46 22.12 -13 16 24.4 "
13.86701 21 46 23.17 -13 16 40.7 "
Sept.18.12032 0 41 12.88 -40 37 46.5 8.0 Debehogne
18.19997 0 41 21.16 -40 37 58.0 "
20.66806 0 46 03.00 -40 38 48.8 Candy
23.70972 0 50 53.66 -40 31 30.0 Jekabsons
28.67467 0 57 04.42 -40 02 16.6 Candy
28.68597 0 57 05.07 -40 02 11.8 "
V. P. Benisek (Belgrade Observatory). 12.5-cm f/8 refractor.
J. Hers (Linden Observatory). Long. = -27o59'34".7, Lat. = -26o07'23".6,
h = 1640 m. The time of the last observation should possibly be
changed by +1 min.
H. Debehogne and R. R. de Freitas Mourao (National Observatory, Rio
de Janeiro).
M. P. Candy and C. Jekabsons (Perth Observatory, Bickley).
Selected total visual magnitude estimates: Sept. 25.22 UT, 6.1
(J. Bortle, Brooks Observatory, 10 x 50 binoculars); 29.25, 6.5
(C. S. Morris, Boalsburg, Pennsylvania, 20 x 80 binoculars); Oct.
1.29, 6.5 (P. Maley, Houston, Texas, 7 x 35 binoculars; tail 0o.7
long in p.a. 340o); 10.25, 6.9 (Maley); 12.26, 7.0 (Maley).
COMET MORI-SATO-FUJIKAWA (1975j)
The following precise positions have been reported:
1976 UT R. A. (1950) Decl. m2 Observer
June 4.67282 21 49 35.75 -68 34 08.3 Gilmore
4.69642 21 49 28.33 -68 34 23.2 "
25.36300 19 41 14.40 -68 57 17.3 14.6 Kilmartin
25.39288 19 41 02.92 -68 56 59.7 "
July 8.71944 18 29 10.90 -65 11 56.1 Candy
Sept.20.52326 17 19 15.19 -40 02 38.3 "
A. C. Gilmore and P. M. Kilmartin (Carter Observatory).
M. P. Candy (Perth Observatory, Bickley). 33-cm astrograph.
AM HERCULIS
S. Tapia, H. Stockman and J. R. P. Angel, University of Arizona,
report that AM Her shows strong circular polarization varying
with the same period of 185m.5 already reported for linear polarization,
photometry and radial velocity (IAUC 2984, 2987). In the R
and V bands the circular polarization varies between +3 percent at
phase 0.1 and -9 percent at phase 0.8 as given by the ephemeris on
IAUC 2987. The circular polarization in the U band is much smaller,
with peak values of +1 percent at phase 0.1 and -0.5 percent at
phase 0.9. It seems likely that the polarization is due to cyclotron
resonance in a field of about 2 x 10**8 gauss.
1976 October 18 (2994) Brian G. Marsden
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