Central Bureau for Astronomical Telegrams
IAUC 4026: RZ Leo; N Vul 1984 No. 2
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 4027
Circular No. 4026
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 617-495-7244/7440/7444
RZ LEONIS
J. Mattei, American Association of Variable Star Observers,
reports that RZ Leo, classified as a 1918 "nova?" (General Cat. of
Var. Stars, Moscow) or a "WZ-Sge-type cataclysmic variable?" (Vogt
and Bateson 1982, A. and Ap. Suppl. Ser. 48, 383), has had an
outburst, as indicated by the following visual magnitude estimates:
1984 Dec. 29 UT, 12.9 (R. Ducoty, Capitola, CA); Dec. 30, 12.9
(Ducoty); 31.52, 12.9 (R. Stanton, La Canada, CA); 1985 Jan. 9.3,
13.0 (C. Scovil, Stamford, CT); 10.3, 13.5: (Scovil).
NOVA VULPECULAE 1984 No. 2
Y. Andrillat, Observatoire de Haute Provence, telexes: "
Spectrograms in the range 355-450 nm (dispersion 40 A/mm) were obtained
on Jan. 2.73 and 3.71 UT with the Haute Provence 1.20-m telescope
and show broad and intense H emission lines [H-gamma up to H10], many
lines of Fe II (multiplets 27, 28, 32), Ti II (multiplets 12, 13,
14, 15, 19, 34, 41, 52, 73, 75), Si II (multiplets 1, 3), and lines
due to Mg II (448.1 nm) and Ca II (396.8 and 393.3 nm). All the
emissions are flanked by two absorption components blue-shifted to
-650 and -1380 km/s. There are two very narrow absorption lines
due to the interstellar calcium. On the spectra taken in the near-
infrared (710-1100 nm), at a dispersion of 230 A/mm on Jan. 3.74,
3.81, 4.72, 4.77, 5.73, and 5.77 UT with the 1.93-m telescope and a
reticon receiver, the nova exhibits the strong emissions of O I
(777.2-777.4-777.5 and 844.6 nm), Ca II (849.8-854.2 and 866.2 nm
blended with the H lines P13, P15, and P16), Mg II (787.7 and 789.6
nm), and relatively weaker emissions due to H (Paschen series from
P6), He I (1083.0 nm), O I (multiplets 8, 34, and 55), C I (1069.1,
904.6, and 965.8 nm), N I (multiplets 1, 2, 3, 19), [N I] (1039.5-
1040.4 nm), and Fe II (771.1 nm). The expansion velocity deduced
from the total width of the O I 777-nm emission line is ~ 1030 km/s.
The equivalent widths of this line and Mg II (787.7-789.6 nm) are,
respectively, 8.8 and 9.6 nm. No changes in the spectrum were
found during the observing period."
Further selected visual magnitude estimates, some provided via
J. Mattei, AAVSO: Jan. 4.05, 6.4 (P. Sventek, Houston, TX); 5.11,
6.2 (C. Womack, Lewisville, TX); 5.960, 6.7 (S. O'Meara, Cambridge,
MA); 6.021, 6.7 (Mattei); 7.03, 6.4 (P. Maley, Houston, TX); 7.77,
6.4 (K. Medway, Southampton, England); 8.10, 6.6 (Womack); 9.10,
6.8 (Womack).
1985 January 11 (4026) Daniel W. E. Green
Read IAUC 4027
Our Web policy. Index to the CBAT/MPC/ICQ pages.
