Circular No. 2854 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 COMET MORI-SATO-FUJIKAWA (1975j) Further precise positions have been reported as follows: 1975 UT R. A. (1950) Decl. Observer Oct. 8.80104 8 23 23.88 + 1 21 07.5 Suzuki 8.80590 8 23 24.01 + 1 20 56.9 " 9.78264 8 24 08.49 + 0 43 28.7 Urata 9.78611 8 24 08.59 + 0 43 22.3 " 9.81632 8 24 10.00 + 0 42 11.2 Suzuki 11.65093 8 25 31.72 - 0 30 03.4 Gilmore 11.66097 8 25 32.15 - 0 30 28.0 " K. Suzuki (JCPM Oi) and T. Urata (Nihondaira Observatory). Measurer: Urata. From Nihondaira Obs. Circ. No. 698. A. C. Gilmore (Carter Observatory). Measurer: P. M. Kilmartin. The following improved orbital elements, by the undersigned, are from 21 observations Oct. 6 to 16: T = 1975 Dec. 25.864 ET Peri. = 246.275 Node = 277.991 1950.0 q = 1.60349 AU Incl. = 91.622 1975 ET R. A. (1950) Decl. Delta r m1 Oct. 25 8 34.12 -10 44.6 1.726 1.806 9.3 30 8 36.59 -15 19.9 Nov. 4 8 38.53 -20 22.4 1.558 1.749 8.9 9 8 39.78 -25 51.9 14 8 40.19 -31 46.6 1.431 1.700 8.6 19 8 39.50 -38 02.2 24 8 37.32 -44 31.8 1.358 1.661 8.4 29 8 33.07 -51 06.2 Dec. 4 8 25.77 -57 34.5 1.347 1.631 8.3 9 8 13.78 -63 45.3 14 7 54.16 -69 26.8 1.394 1.612 8.3 m1 = 5.5 + 5 log Delta + 10 log r Selected total visual magnitude estimates: Oct. 14.43 UT, ~ 9 (D. Green and T. Rokoske, Boone, North Caro1ina, 20-cm f/6 reflector); 18.47, 10.0 (B. Hudgens, Clinton, Mississippi, 25-cm f/6 reflector); 19.48, 10.0 (P. Maley, Houston, Texas, 13-cm f/5 refractor); 21.41, 9.5 (J. Bortle, Brooks Observatory, 32-cm reflector). R CORONAE BOREALIS Independent communications from the Variable Star Section of the British Astronomical Association and from the American Association of Variable Star Observers show that this star has started to decline in brightness. Visual magnitude estimates are: Oct. 3.05 UT, 5.9 (G. Kelley); 14.01, 6.2 (Kelley); 14.78, 6.6 (M. Hapgood); 15.78, 6.7 (J. Isles); 20.99, 7.0 (Kelley); 21.99, 7.2 (M. Mattei); 22.1, 7.2 (J. Bortle). 3U 0352+30 N. E. White, K. O. Mason and P. W. Sanford, Mullard Space Science Laboratory, report that four Copernicus observations of 3U 0352+30 (= X Per) show that the 2.5-7.5 keV flux is pulsed with a period of 13.924 +/- 0.007 min, stable to within 0.027 min over 3 years. The peak to mean amplitude is 37 percent, constant to within 5 percent. NOVA MONOCEROTIS 1975 R. F. Jameson, Astronomy Department, Leicester University, reports the following 2.2-um magnitudes, obtained using the 152-cm telescope on Tenerife: Sept. 24-25, 9.9; Oct. 1.13, 10.46; 3.13, 10.38. The errors are 3.2, 2.6 and 3.0 sigma, respectively. E. L. Robinson and R. E. Nather, Department of Astronomy, University of Texas at Austin, write: "The x-ray nova was observed in white light with the high-speed photometer at McDonald Observatory on Oct. 10 UT. The light curve was analyzed for both random and periodic luminosity variations on timescales between 2 and 200 sec. There were no random variations with amplitudes greater than 0.01 magnitude and no periodic variations with amplitudes greater than 0.001 magnitude." J. Bortle provides the following visual magnitude estimates: Oct. 3.40, 11.9; 4.35, 11.9; 8.38, 11.9; 21.41, 12.2; 22.40, 12.2. 1973 EC E. Roemer, University of Arizona, communicates the following precise positions, obtained by R. McCallister and herself with the Steward Observatory's 229-cm reflector. Measurer: C. C. McCarthy. 1975 UT R. A. (1950) Decl. Aug. 8.41092 2 25 02.55 +25 00 56.3 8.43368 2 25 04.20 +25 01 07.8 1975 October 23 (2854) Brian G. Marsden
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