Central Bureau for Astronomical Telegrams
IAUC 2722: 433 EROS; N Per 1974; JUPITER I (IO)
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Read IAUC 2723
Circular No. 2722
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
433 EROS
Dr. R. S. Harrington, U.S. Naval Observatory, Washington,
provides the following precise positions, obtained with the 38-cm
astrograph (stopped down to 23-cm):
1974 UT R. A. (1950) Decl.
Nov. 9.23889 6 38 14.67 +54 52 15.8
18.16458 7 04 14.09 +56 04 00.9
18.17986 7 04 16.54 +56 04 07.9
The following orbital elements, by the undersigned, are based
on 147 observations 1961 Apr. 11 to 1974 Nov. 18. Perturbations by
Mercury to Pluto were considered; the mean residual is 0".99.
T = 1975 Jan. 24.70450 ET Epoch = 1975 Jan. 28.0 ET
Peri. = 178.44991 e = 0.2227021
Node = 303.83085 1950.0 a = 1.4579641 AU
Incl. = 10.82772 n = 0.55986565
q = 1.1332725 P = 1.760 years
These elements yield the following improved prediction for the
occultation of kappa Gem A on 1975 Jan. 24.0 UT (cf. IAUC 2695):
UT Long. Lat. UT Long. Lat. UT Long. Lat.
0h15m2 +96o4 +55o0 0h19m2 +71o9 +46o0 0h29m5 +59o0 +15o0
0 15.9 +90.2 +54.0 0 19.6 +70.7 +45.0 0 31.1 +59.2 +10.0
0 16.4 +86.2 +53.0 0 19.9 +69.6 +44.0 0 32.6 +59.8 + 5.0
0 16.9 +82.9 +52.0 0 20.3 +68.6 +43.0 0 34.0 +60.7 0.0
0 17.3 +80.2 +51.0 0 21.3 +66.1 +40.0 0 35.3 +62.0 - 5.0
0 17.7 +78.0 +50.0 0 23.0 +63.0 +35.0 0 36.5 +63.8 -10.0
0 18.1 +76.2 +49.0 0 24.7 +61.0 +30.0 0 37.6 +66.1 -15.0
0 18.5 +74.6 +48.0 0 26.3 +59.8 +25.0 0 38.6 +68.9 -20.0
0 18.8 +73.2 +47.0 0 27.9 +59.2 +20.0 0 39.5 +72.5 -25.0
This track could still be in error by up to +/- 100 km. Further
high-quality astrometric observations during December and January will
definitely be useful for improving the prediction. We should be
glad to receive these at the Central Bureau, although since it seems
inappropriate to include a large number of positions of a
well-known minor planet on these Circulars, we reserve the right to
withhold them from publication. Contributors should therefore also
send their observations to the Minor Planet Center, Cincinnati
Observatory, Observatory Place, Cincinnati, Ohio 45208, U.S.A.
NOVA PERSEI 1974
Mr. C. Y. Shao, Center for Astrophysics, Harvard and Smithsonian
Observatories, provides the following precise position, measured
from a plate taken with the 40-cm Metcalf astrograph at the
Agassiz Station: R.A. = 3h04m12s.47, Decl. = +46o56'09".8 (equinox 1950.0).
Examination of the Palomar Sky Survey prints shows that there is a
faint blue star, mpg ~ 19.5, at the position of the nova.
Mr. Shao also reports that images of the nova appear on patrol
plates taken with the Damon cameras at Agassiz as long ago as September.
He gives the following magnitude estimates, the last two
of them from post-discovery plates with the Metcalf astrograph:
1974 UT mpg 1974 UT mpg 1974 UT mpg
Aug. 17.287 >14 Oct. 9.359 11.3 Nov. 15.175 11.5
Sept.16.313 10.0 19.278 10.5 17.191 11.5
24.310 8 Nov. 11.226 11.4
The following visual (or pv) magnitude estimates are available:
1974 UT mv Observer 1974 UT mv Observer
Nov. 13.84 11.4 Diethelm Nov. 16.0 11.2 Bortle
13.84 11.5 Locher 17.1 11.3 "
14.78 11.4 Dietheim 19.0 11.3 "
14.78 11.5 Locher 20.0 10.6 M. Taylor
15.1 10.8 Scovil (pv) 20.0 10.8 P. Taylor
15.83 11.2 Locher 21.0 10.8 "
R. Diethelm and K. Locher (Wetzikon, Switzerland). Comparison star
No. 2972 in U.S.N.O. Photoelectric Catalogue (R.A. =3h02m.1, Decl. =
+49o39', equinox 1950.0): assumed V = 11.70.
C. Scovil (Stamford, Connecticut), Mary Jane Taylor and P. Taylor
(Boynton Beach, Florida). Using provisional AAVSO chart based
on McCormick photovisual sequence (Wirtanen and Vyssotsky 1945,
Astrophys. J. 101, 141). Communicated by Janet Mattei. Scovil
has independently identified the prenova with the faint blue
star mentioned above.
J. Bortle (Brooks Observatory). Compromise between provisional
AAVSO chart and magnitude sequences from other fields.
JUPITER I (IO)
D. P. Cruikshank, C. B. Pilcher and W. M. Sinton, University
of Hawaii, write: "Helium emission at 10 830 A reported earlier
(IAUC 2693) has been found to be due to scattered light from a He-Ne
laser incorporated in the observing equipment. There is no
observational evidence for He emission in the vicinity of Io."
1974 November 25 (2722) Brian G. Marsden
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