Central Bureau for Astronomical Telegrams
IAUC 3005: N Vul 1976; N Oph 1976; EMISSION Var IN Sge; 1976 UA; MIRANDA APPULSE ON 1977 Mar. 10; TIME ADJUSTMENT ON 1976 Dec. 31
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Read IAUC 3006
Circular No. 3005
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
NOVA VULPECULAE 1976
Y. Andrillat and C. Fehrenbach, Haute Provence Observatory,
report that spectrograms of range 5900-12 000 A (dispersion 230 A/mm)
and range 3800-5000 A (dispersion 80 A/mm) show emissions from H-alpha
to H9, Fe II, Ca II (including the infrared triplet), very intense
O I 8446 and 7772 A, N I, C I, Si I, Si II, Na I, Mg II, [O I]
6300 and 6363 A and [N I] 10 394-10 404 A. On the blue plate the
broad emissions (velocity 1350 km/s) are bordered by absorption systems
at -1040 km/s and (less intense) at -560 km/s. Absorptions of
Ti II, Mg II, Si II, Ca II and probably Mg I and O I are identified.
G. Klare and B. Wolf, Landessternwarte, Heidelberg-Konigstuhl,
report that on Nov. 8.77 UT the spectrum in the blue (dispersion 55
A/mm) was characterized by very broad and intense H and metallic
(Fe II, Ti II) emission lines. In addition to the principal
absorption spectrum strong diffuse enhanced absorption lines were found
from H-beta to H-delta with a velocity of about -2000 km/s.
The following photoelectric observations have been reported:
1976 UT V Observer 1976 UT V Observer
Oct. 22.85 6.88 Di Paolantonio Nov. 5.01 8.23 Whitney
28.75 7.09 " 6.02 8.56 Landis
Nov. 2.01 6.68 Landis 9.05 7.85 Whitney
3.02 6.64 " 11.02 7.72 "
4.00 7.70 "
A. Di Paolantonio (Collurania Observatory). Comparison star BD
+19 4028 (assumed V = 6.90). Communicated by P. Tempesti.
H. Landis (East Point, Georgia). Communicated by J. Mattei.
C. A. Whitney (Harvard College Observatory, Agassiz Station). B-V
= +1.22 on Nov. 5, +1.04 on Nov. 9 and +1.12 on Nov. 11.
Comparison star HD 182293 (assumed V = 7.14, B-V = +1.15).
NOVA OPHIUCHI 1976
Japan Astron. Circ. No. 74 gives the following precise position
by T. Urata, JCPM Yakiimo Station: R.A. = 18h01m05s.19, Decl. =
+11o47'46".0 (equinox 1950.0). Yamamoto Circ. No. 1839 gives a very
similar position by T. Kurosaki (end figures 05s.19, 47".5).
EMISSION VARIABLE IN SAGITTA
L. J. Chaisson (nee Eachus), Center for Astrophysics, communicates
the following photographic magnitudes for this object (cf.
IAUC 2995), derived from Harvard patrol plates: 1975 May 8, 13.2;
11, 13.3; July 4, 12.3; Aug. 5, 11.4; Sept. 3, 11.5; Oct. 7, 11.7;
31, 12.0; 1976 Mar. 22, 12.0; June 2, 11.1; Sept. 28, 12.4; Oct. 23,
12.5. The object must have been fainter than magnitude 16 during
l934-1964, fainter than magnitude 14 during 1923-1933 and than
magnitude 13 during 1915-1922; earlier plates, extending back to 1894,
have not been thoroughly checked. Dokuchaeva (1976, Inf. Bull.
Variable Stars No. 1189) reports similar results, obtained from the
plate collection at the Sternberg Astronomical Institute.
1976 UA
Further positions have been reported as follows:
1976 UT R. A. (1950) Decl. mpg Observer
Oct. 27.20293 0 07 23.21 - 1 00 55.9 McCrosky
29.06179 0 11 36.54 - 2 39 44.9 "
29.22500 0 11 51.75 - 2 46 08.4 Giclas
29.24792 0 11 53.10 - 2 46 58.9 "
30.32431 0 13.54 - 3 23.8 16.8 Roemer
30.34792 0 13.56 - 3 24.5 "
R. E. McCrosky (Harvard College Observatory). Measurer: C. Y. Shao.
H. L. Giclas (Lowell Observatory). Measurer: M. L. Kantz.
E. Roemer (Lunar and Planetary Laboratory). 154-cm reflector.
MIRANDA APPULSE ON 1977 MARCH 10
R. J. Greenberg, Planetary Science Institute; and W. B.
Hubbard, University of Arizona, write: "The occultation of BD -14
3996 = SAO 158687 by Uranus on 1977 Mar. 10 will be followed by an
appulse of Uranus V (Miranda) to the star at about 23h34m UT. The
apparent orbital longitude of the satellite (measured from the
ascending node on the ecliptic) is then predicted to be 184o +/- 1o, as
deduced from a theory for Miranda's orbit and 17 longitude measurements
obtained by R. L. Walker and J. W. Christy at the U.S. Naval
Observatory during the 1975 apparition. Assuming the correctness
of the published ephemeris for Uranus, we find that Miranda's
shadow will pass to the north of the earth's center with a closest
approach distance of about 12 000 km. An occultation is thus unlikely
to be observed from the earth, although a spacecraft observation
may be possible. The appulse will be observable from India, the
Middle East and Africa. None of the other Uranian satellites will
yield an occultation observable from the vicinity of the earth."
TIME ADJUSTMENT ON 1976 DECEMBER 31
The Bureau International de 1'Heure informs us that a positive
leap second will occur such that the sequence of UTC second markers
will be: 1976 Dec. 31d23h59m59s, 31d23h59m60s, 1977 Jan. 1d00h00m00s.
1976 November 12 (3005) Brian G. Marsden
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