Central Bureau for Astronomical Telegrams
IAUC 2740: P/WOLF; GK Per; BINARY PULSAR
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Read IAUC 2741
Circular No. 2740
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
PERIODIC COMET WOLF
The following practically identical sets of elements were
derived by E. I. Kazimirchak-Polonskaya, Institute for Theoretical
Astronomy, Leningrad, and by D. K. Yeomans, Computer Sciences
Corporation, from observations 1925-1967. Perturbations by Mercury
to Pluto were taken into account, and nongravitational effects were
found to be negligible. The ephemeris is by Mrs.
Kazimirchak-Polonskaya.
Kazimirchak-Polonskaya Yeomans
Epoch = 1976 Jan. 23.0 1976 Jan. 23.0 ET
T = 1976 Jan. 25.3573 1976 Jan. 25.3563 ET
Peri. = 161.1453 161.1452
Node = 203.8087 203.8086 1950.0
Incl. = 27.3319 27.3320
q = 2.500775 2.500771 AU
e = 0.395684 0.395685
a = 4.138193 4.138192 AU
n = 0.1170814 0.1170815
P = 8.418 8.418 years
1975/76 ET R. A. (1950) Decl. Delta r m2
Mar. 19 20 02.32 + 3 49.6 3.630 3.203 20.9
29 20 14.32 + 5 20.1
Apr. 8 20 25.64 + 6 57.1 3.351 3.132 20.6
18 20 36.13 + 8 39.6
28 20 45.68 +10 26.3 3.059 3.064 20.3
May 8 20 54.14 +12 15.7
18 21 01.33 +14 06.0 2.766 2.996 20.0
28 21 07.08 +15 54.7
June 7 21 11.22 +17 39.1 2.488 2.931 19.6
17 21 13.56 +19 15.3
27 21 14.00 +20 39.0 2.238 2.869 19.3
July 7 21 12.48 +21 45.0
17 21 09.11 +22 27.6 2.034 2.810 19.0
27 21 04.22 +22 41.8
Aug. 6 20 58.34 +22 23.4 1.894 2.754 18.8
16 20 52.21 +21 31.0
26 20 46.69 +20 06.6 1.832 2.702 18.6
Sept. 5 20 42.55 +18 15.6
15 20 40.42 +16 06.2 1.854 2.656 18.6
25 20 40.70 +13 47.7
Oct. 5 20 43.52 +11 29.0 1.952 2.614 18.6
15 20 48.86 + 9 17.7
25 20 56.54 + 7 19.2 2.110 2.579 18.7
Nov. 4 21 06.29 + 5 37.0
14 21 17.87 + 4 13.2 2.306 2.549 18.9
24 21 30.97 + 3 08.2
Dec. 4 21 45.35 + 2 21.8 2.523 2.527 19.0
14 22 00.77 + 1 53.0
24 22 17.01 + 1 40.5 2.743 2.511 19.2
Jan. 3 22 33.90 + 1 42.6
13 22 51.30 + 1 57.5 2.954 2.503 19.3
23 23 09.07 + 2 23.3
Feb. 2 23 27.13 + 2 58.2 3.145 2.502 19.5
12 23 45.39 + 3 40.3
22 0 03.80 + 4 27.7 3.307 2.509 19.6
m2 = 13.0 + 5 log Delta + 10 log r
GK PERSEI
Dr. K. Osawa, Director of the Tokyo Astronomical Observatory,
reports that an outburst of this nova has been discovered by K.
Hirosawa and confirmed by Y. Hirasawa. Recent visual magnitude
estimates, including some communicated by Mrs. Janet Mattei,
American Association of Variable Star Observers, are as follows:
Jan. 14.1 UT, 13.1 (C. Hurless); 15.1, 13.2 (Hurless); 17.1, 13.1
(Hurless); 19.1, 12.9 (Hurless); 20.50, 12.0 (Hirosawa); 20.59,
12.2 (Hirasawa); 21.14, 12.6 (Hurless); 22.15, 11.8 (E. Mayer);
22.19, 12.0 (R. Annal).
BINARY PULSAR
H. W. van Someren Greve, Leiden Observatory; H. van der Laan,
Leiden Observatory and Institute for Advanced Study, Princeton; and
J. W. M. Baars, Westerbork Observatory, write: "We have detected a
source in the 2' by 2' error box of the Taylor-Hulse binary pulsar
(IAUC 2704) in a 12-hr measurement on SD 74284 at 1415 MHz with the
Westerbork Synthesis Radio Telescope. The position is R.A. =
19h13m12s.0 +/- 0s.3, Decl. = +16o00'18" +/- 18" (equinox 1950.0), and the
flux density is 1.9 +/- 0.5 mJy. The probability of a chance
coincidence within the error box previously reported by the pulsar
discoverers is less than 10 percent. There is no evidence for any
supernova remnant of surface brightness greater than 2 x 10**-22 W
m**-2 Hz**-1 sr**-1. A more critical search for the supernova remnant
and another pulsar flux determination are to be made at 610 MHz."
1975 January 24 (2740) Brian G. Marsden
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