Central Bureau for Astronomical Telegrams
IAUC 2707: N Sgr 1974; SN IN NGC 7343; SU Tau; U Cep; 1974c
The following International Astronomical Union Circular may be linked-to from your own Web pages, but must not otherwise be redistributed (see these notes on the conditions under which circulars are made available on our WWW site).
Read IAUC 2708
Circular No. 2707
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
NOVA SAGITTARII 1974
Dr. K. Osawa, Director of the Tokyo Astronomical Observatory,
cables that Yoshiyuki Kuwano, Hita, Oita, has observed a new, but
unconfirmed, object as follows:
1974 UT R. A. (1950) Decl. mv
Oct. 6.44167 17 45.7 -18 45 9.0
The object, presumably a nova, was confirmed on Oct. 11.0 UT by K.
Simmons and R. Sweetsir (Florida) and C. Sherrod (Arkansas). The
following magnitude estimates are available: Oct. 11.04, 9.4
(Simmons); 11.04, 9.2 (Sweetsir); 11.05, 9.1-9.2 (Sherrod); 12.05,
9.5 (Simmons); 12.05, 9.3 (Sweetsir).
SUPERNOVA IN NGC 7343
Dr. L. Rosino, Director of the Asiago Astrophysical Observatory,
cables that he has discovered a supernova 10" east and 17"
south of the nucleus of NGC 7343 (R.A. = 22h36m.3, Decl. = +33o48', equinox
1950.0). On Oct. 9.95486 UT the photographic magnitude was 15.5.
SU TAURI
Mr. C. Scovil, Stamford Museum, Connecticut, reports that this
R CrB variable was estimated at magnitude 14.1 on Oct. 8.3 UT. It
had been fainter than magnitude 15 since Oct. 1973 (cf. IAUC 2583).
U CEPHEI
Dr. M. Plavec, University of California at Los Angeles, writes:
"The strong emission lines reported by Batten et al. (IAUC 2701)
were observed as early as Aug. 8 by M. Plavec, R. S. Polidan and
H. L. Burger at the Lick Observatory. The relatively high dispersion
(17 A/mm) and time resolution (10-20 min) of the Varo image
intensifier attached to the 305-cm telescope permitted us to follow
the H-alpha emission on ten plates. Just prior to the onset of totality,
the red emission lobe was extremely strong, while the violet lobe
was marginal. At mid-totality, the red lobe was weaker and the
violet lobe equally strong. Just after the end of totality, the
shape of the emission was approximately a mirror image of that
before totality. The emissions were then observed for another 80 min,
during which time the violet lobe decreased in intensity almost to
zero, while the red lobe was barely present. The absorption core
was always rather deep and narrow. Concurrent seven-color photometric
observations by L. McDonald (of the University of California
at Santa Cruz) gave Aug. 8.435 UT as a first approximation to the
heliocentric time of minimum; the duration of totality at 6300 A was
about 80 min, but there were distortions at both ends that are possibly
due to the emissions. Evidently, U Cep recently developed a
ring or disk that is qualitatively very similar to that in Joy's
well-known model for RW Tau; Batten's observations during the past
few years suggested only a luminous bridge between the two components.
If this is a result of a major outburst, timing of minima
may reveal a jump in the period."
COMET LOVAS (1974c)
The following improved parabolic elements, by the undersigned,
are from 50 observations Mar. 21 to June 9:
T = 1975 Aug. 22.1731 ET Peri. = 261.3409
Node = 11.6699 1950.0
q = 3.012426 AU Incl. = 50.6363
1974/75 ET R. A. (1950) Decl. Delta r m2
Nov. 29 13 47.10 -26 36.2 4.733 3.959 16.4
Dec. 9 13 56.70 -28 45.6
19 14 06.23 -31 00.9 4.421 3.841 16.1
29 14 15.56 -33 22.5
Jan. 8 14 24.57 -35 51.0 4.072 3.728 15.8
18 14 33.09 -38 27.1
28 14 40.89 -41 11.2 3.706 3.621 15.4
Feb. 7 14 47.73 -44 03.7
17 14 53.23 -47 04.6 3.349 3.519 15.1
27 14 56.95 -50 13.0
Mar. 9 14 58.32 -53 27.3 3.028 3.424 14.8
19 14 56.57 -56 43.9
29 14 50.81 -59 57.3 2.768 3.337 14.4
Apr. 8 14 40.08 -62 59.9
18 14 23.57 -65 41.4 2.586 3.258 14.2
28 14 01.34 -67 51.2
May 8 13 34.89 -69 20.6 2.491 3.189 14.0
18 13 07.4 -70 06.9
28 12 42.9 -70 16.1 2.473 3.130 13.9
June 7 12 24.30 -69 59.7
17 12 12.80 -69 31.3 2.515 3.083 13.9
27 12 08.28 -69 02.3
July 7 12 10.36 -68 40.6 2.595 3.047 13.9
m2 = 7.0 + 5 log Delta + 10 log r
The total magnitude m1 could reach 10 or brighter in July.
1974 October 15 (2707) Brian G. Marsden
Read IAUC 2708
Our Web policy. Index to the CBAT/MPC/ICQ pages.
