Central Bureau for Astronomical Telegrams
IAUC 3102: 1977l; JUPITER XIII (LEDA); CH Cyg
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Read IAUC 3103
Circular No. 3102
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 Telex: 921428
Telephone: (617) 864-5758
PERIODIC COMET CHERNYKH (1977l)
The following precise positions have been reported:
1977 UT R. A. (1950) Decl. m1 Observer
Aug. 24.05278 0 19 58.39 - 3 25 57.3 14 Chernykh
25.03912 0 19 49.54 - 3 29 53.3 14 "
Sept. 2.63438 0 17 49.96 - 4 08 07.3 14 Jekabsons
4.60417 0 17 12.12 - 4 17 46.4 14 Candy
5.65938 0 16 50.22 - 4 23 03.0 14 "
N. S. Chernykh (Crimean Astrophysical Observatory). Communicated
by G. R. Kastel' (I.T.A., Leningrad) and E. P. Aksenov (Sternberg
Astronomical Institute). The name of Yu. P. Pskovskij was
accidentally omitted as a communicator on IAUC 3100.
P. Jekabsons and M. P. Candy (Perth Observatory, Bickley). 33-cm
astrograph. Comet diffuse with condensation.
Candy also communicates the following elliptical orbit, from
observations Aug. 24 to Sept. 5. His ephemeris has been extended.
T = 1978 Jan. 2.902 ET
Peri. = 255.63 e = 0.5228
Node = 132.23 1950.0 a = 5.5321 AU
Incl. = 5.45 n = 0.07575
q = 2.6399 AU P = 13.01 years
1977 ET R. A. (1950) Decl. Delta r m1
Aug. 25 0 19.85 - 3 29.6 1.913 2.820 13.9
Sept. 4 0 17.41 - 4 14.8 1.834 2.795 13.8
14 0 13.45 - 5 06.6 1.779 2.771 13.7
24 0 08.54 - 5 59.5 1.750 2.749 13.6
Oct. 4 0 03.42 - 6 47.2 1.747 2.729 13.6
14 23 58.88 - 7 24.2 1.770 2.711 13.6
m1 = 8.0 + 5 log Delta + 10 log r
JUPITER XIII (LEDA)
K. Aksnes, Center for Astrophysics, provides the following
continuation to the ephemeris on IAUC 2968:
1977/78 ET R. A. (1950) Decl. dR.A. dDecl. Delta r
Aug. 25 5 58.80 +23 17.0 -2m77 +14'6 5.534 0.071
Sept. 4 6 05.82 +23 11.9 -2.38 + 9.9 5.410 0.068
14 6 12.12 +23 04.9 -1.79 + 3.9 5.275 0.065
24 6 17.56 +22 56.5 -1.01 - 3.0 5.131 0.063
Oct. 4 6 21.98 +22 48.0 -0.07 -10.2 4.979 0.062
14 6 25.18 +22 40.7 +0.96 -16.9 4.822 0.062
24 6 26.95 +22 35.7 +1.95 -22.0 4.666 0.064
Nov. 3 6 27.15 +22 33.8 +2.82 -25.0 4.517 0.066
13 6 25.68 +22 35.3 +3.45 -25.4 4.380 0.069
23 6 22.57 +22 39.9 +3.78 -23.3 4.264 0.072
Dec. 3 6 18.00 +22 47.0 +3.78 -19.1 4.172 0.076
13 6 12.26 +22 55.6 +3.45 -13.2 4.112 0.079
23 6 05.79 +23 04.6 +2.82 - 6.4 4.085 0.081
Jan. 2 5 59.10 +23 13.2 +1.97 + 0.6 4.094 0.083
12 5 52.74 +23 20.7 +0.99 + 7.3 4.139 0.085
22 5 47.20 +23 26.9 -0.01 +13.1 4.217 0.086
Feb. 1 5 42.87 +23 32.1 -0.96 +17.8 4.324 0.087
11 5 40.01 +23 36.3 -1.77 +21.4 4.455 0.087
21 5 38.76 +23 39.9 -2.43 +23.7 4.607 0.087
Mar. 3 5 39.12 +23 42.9 -2.92 +24.9 4.772 0.086
13 5 41.06 +23 45.3 -3.22 +25.0 4.945 0.084
23 5 44.47 +23 46.8 -3.36 +24.1 5.122 0.082
Apr. 2 5 49.20 +23 47.1 -3.34 +22.2 5.298 0.079
12 5 55.13 +23 45.9 -3.16 +19.2 5.469 0.076
22 6 02.10 +23 42.7 -2.85 +15.2 5.630 0.073
CH CYGNI
Ch. Fehrenbach, Haute Provence Observatory, reports: "CH Cyg
was observed on Sept. 2, 3 and 4 by Y. Andrillat and R. Faraggiana
in the red and near infrared (range 5800-11 000 A, dispersion 230
A/mm, 193-cm and 120-cm telescopes) and in the blue-green (range
3400-5030 A, dispersion 12.4 A/mm, 152-cm telescope). In the blue
region a continuum comparable to that observed in 1967 is present.
From visual inspection it appears that the Balmer series, detectable
to about H18, is present in absorption with emission wings,
broader on the violet side. The emission wings of the H and K
lines of Ca II are broader on the red side. He I 5016 A and 3888 A
(metastable levels) and [S II] 4068 A are present in emission. Fe
II 4233 A emission has an intensity comparable to that of [Fe II]
4243 A. Weak, sharp emission lines are visible on the violet side
of the Balmer jump. The red and near-infrared regions are
dominated by the strong molecular bands of TiO at 8859, 8432, 8344,
7828, 7672, 7628, 7589, 7198, 7126, 7088, 7054, 6651, 6158 and
5809 A. Only H-alpha is present in emission. Two lines of the Ca II
triplet (8662 and 8542 A) are visible, the third being blended with
a TiO band. It is interesting to remark that athough the metastable
lines are present, He I 10 830 A is not visible on our spectrograms.
No other lines of He I are visible, and they are probably
too faint to be detected on small-dispersion spectrograms."
1977 September 7 (3102) Brian G. Marsden
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