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IAUC 5685: 1992 QB1; SATURN VI (TITAN); GRO J0422+32

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IAUC number 

                                                  Circular No. 5685
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@CFA or GREEN@CFA (.SPAN, .BITNET or .HARVARD.EDU)


1992 QB1
     Ephemeris continuation from the orbital elements on IAUC 5684:

1993 TT     R. A. (2000) Decl.     Delta      r    Elong. Phase      V
Jan.  3    23 56.04    - 0 23.6   41.045   40.822   76.2    1.3     23.8
     13    23 56.47    - 0 20.7   41.207   40.820   66.1    1.3     23.8
     23    23 57.04    - 0 16.9   41.358   40.818   56.1    1.1     23.8


SATURN VI (TITAN)
     B. Bezard and A. Marten, Observatoire de Paris-Meudon; and G.
Paubert, Institut de Radio Astronomie Millimetrique, communicate: "We
report the first detection of CH_3CN on Titan, using the IRAM 30-m radio
telescope at Pico Veleta.  The J=12-11 multiplet of CH_3CN around 220.7
GHz was observed at 0.1-MHz resolution on Dec. 25-27.  During this run
we also reobserved at the same spectral resolution the (24-23) line of
HC_3N that we first detected in May.  For both molecules the line
width (FWHM) is approximately 400 KHz, implying that the lines are
formed in the doppler regime and originate from the upper stratosphere
or mesosphere of Titan.  A first analysis of these observations, based
on radiative-transfer calculations, indicates that the disk-averaged
column abundance of CH_3CN above 300 km is larger than that of HC_3N.
These two millimeter observations impose stringent constraints on
photochemical models of Titan."


GRO J0422+32
     B. A. Harmon and G. J. Fishman, NASA Marshall Space Flight Center;
and W. S. Paciesas, University of Alabama, Huntsville, report for the
BATSE/CGRO Experiment Team: "Hard x-ray monitoring (cf. IAUC 5580, 5584,
5587, 5592, etc.) using earth occultation indicates that flux from GRO
J0422+32 in the 20-300-keV energy band exhibits a secondary maximum
similar to those of other x-ray novae.  An upward turn in the hard x-ray
flux began about Dec. 1, with the flux level at approximately 150 mCrab,
which then increased to a peak of about 500 mCrab on Dec. 20.  During
Dec. 20-27 it dropped to about 400 mCrab.  Prior to Dec. 1, the flux had
been decreasing exponentially (time constant = 40.4 days) since the
primary outburst in August.  Fits to an optically-thin thermal
bremsstrahlung model before and during the recent intensity increase
yield average temperatures of 136 +/- 8 keV (Nov. 24-Dec. 1) and 122
+/- 4 keV (Dec. 15-22), respectively."


1992 December 30               (5685)              Brian G. Marsden

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