Central Bureau for Astronomical Telegrams
IAUC 3498: COMET CHERNYKH-PETRAUSKAS; 59 Cyg; NEAR-IR Obs OF EMISSION OBJECTS
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Read IAUC 3499
Circular No. 3498
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
TWX 710-320-6842 ASTROGRAM CAM Telephone 617-864-5758
COMET CHERNYKH-PETRAUSKAS
Yu. P. Pskovskij, Sternberg Astronomical Institute, Moscow,
cables that Chernykh and Petrauskas have discovered a comet, as
follows:
1980 UT R. A. (1950) Decl. m1
July 31.708 11 50.0 +32 40 9
The daily motion is 20' eastward. Nothing was reported about the
comet's appearance. No other observations have been recieved.
59 CYGNI
P. K. Barker, Department of Astronomy, University of Western
Ontario, reports intensifier-dissector-scanner observations of
rapidly increasing infrared emission in the early-Be star 59 Cyg
(= V832 Cyg = HR 8047). On June 23 an almost flat continuum was
seen in the 850-nm region, but on July 25 the Paschen lines P13-P17
were observed in emission above the continuum at intensity 1.1,
with unusual flat-topped profiles of width 600 km/s. There is an
asymmetric emission feature at O I 844.6 nm. H-alpha emission has
maintained intensity 1.6 from Apr. 22 to July 25. The latest observations
show only a very weak central absorption in the continuum at H-beta and
partial filling of H-gamma by asymmetric emission. H-delta, H-epsilon and
H-beta retain photospheric appearance. Observers are urged to follow
the star at all possible wavelengths.
NEAR-INFRARED OBSERVATIONS OF EMISSION OBJECTS
Y. Andrillat, Observatoire de Haute Provence; and J. P. Swings,
Institut d'Astrophysique, Liege, telex: "Observations performed during
the night of July 13-14 with the Haute Provence 1.93-m telescope
and the near-infrared spectrograph (dispersion 23 x 10**-6)
equipped with a reticon reveal the following striking spectral
modifications in emission-line strengths compared to data obtained one
year ago under similar conditions: an increase by about a factor of
three of O I 844.6 nm in V1016 Cyg; the appearance of He II 1012.3
nm in HM Sge with a strength slightly greater than that of the
neighboring P7; and an increase by about a factor of two of O I
844.6 nm in MWC 349A (the brighter component). Except for minor
changes, the other emission lines have remained unchanged.
Observations in other wavelength regions should be undertaken."
1980 August 4 (3498) Brian G. Marsden
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