Central Bureau for Astronomical Telegrams
IAUC 6455: 1996 Q1; GRS 1915+105
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Circular No. 6455
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
BMARSDEN@CFA.HARVARD.EDU or DGREEN@CFA.HARVARD.EDU (science)
Phone 617-495-7244/7440/7444 (for emergency use only)
COMET 1996 Q1
Vello Tabur, Wanniassa, Australian Capital Territory, reports
his discovery of a comet. The following observations are available:
1996 UT R.A. (2000) Decl. m1 Observer
Aug. 19.6951 4 44 30 - 9 23.2 10 Tabur
19.8000 4 44 42 - 9 22.4 "
20.7361 4 46 12 - 9 02.9 "
21.10556 4 46 44.91 - 8 55 52.2 11.1 Mikuz
21.11506 4 46 45.85 - 8 55 41.1 "
21.12133 4 46 46.38 - 8 55 36.9 "
21.12574 4 46 46.78 - 8 55 28.3 "
21.45 4 47.5 - 8 49 10.0 Hale
V. Tabur (Wanniassa, A.C.T.). 0.20-m f/4.7 reflector. Circular
coma of diameter 3' with little or no condensation.
H. Mikuz (Crni Vrh Observatory). 0.20-m f/2 Baker-Schmidt telescope
+ CCD + V filter. Coma diameter 4'.5, moderately condensed.
A. Hale (Cloudcroft, NM). 0.41-m reflector (visual). Coma
diameter 3'.5.
GRS 1915+105
B. Sams and A. Eckart, Max-Planck-Institut fur
Extraterrestrische Physik; and R. Sunyaev, Max-Planck-Institut fur
Astrophysik, report the disappearance of the near-infrared jets
observed in GRS 1915+105 in July 1995 (Sams et al. 1996, Nature 382,
47): "Using the same observing equipment as in July 1995 (ESO New
Technology Telescope + SHARP speckle camera), new observations on
June 7 show no evidence of any asymmetry in the image of the object
down to a 3-sigma level of (magnitude) K = 16.5 +/- 0.3. This is a
factor of eleven times fainter than the previously observed
southwest jet. Hence the lifetime of the infrared jet is < 1 yr.
We detected the brightest total infrared emission yet observed from
GRS 1915+105, with J = 16.3 +/- 0.1, H = 14.0 +/- 0.1, and K = 12.3
+/- 0.1. Fluxes were calibrated against kappa Aql (HR 7446), which
was assumed to have J = 5.03, H = 5.06, and K = 5.07. Comparison
with previous observations (IAUC 6267; Mirabel et al. 1995, A.Ap.
282, L17) shows that the infrared emission from GRS 1915+105
becomes bluer as the K-band emission increases. This behavior is
typical of systems with x-ray heating of the normal star and outer
zones of the accretion disk."
(C) Copyright 1996 CBAT
1996 August 21 (6455) Daniel W. E. Green
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