THE ASTRONOMER Electronic Circular No 715 1993 Mar 06 16.33UT
Ed:Guy M Hurst, 16,Westminster Close, Kempshott Rise, Basingstoke,
Hants, RG22 4PP,England. Telephone/FAX(0256)471074 Int:+44256471074
TELEX: 9312111261 Answerback: TA G TELECOM GOLD: 10074:MIK2885
GMH at UK.AC.RUTHERFORD.STARLINK.ASTROPHYSICS STARLINK: RLSAC::GMH
GMH at UK.AC.CAM.ASTRONOMY.STARLINK STARLINK: CAVAD::GMH
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SUPERNOVA 1993F IN ANONYMOUS GALAXY
C. Pollas reports his discovery of an apparent supernova of mag
about 18.5 on two technical pan films (limiting mag 21-22) taken
Jan. 18.97 and 20.94 UT by D. Albanese and himself with the 0.9-m
Schmidt telescope at the Observatoire de la Cote d'Azur. The
candidate, at R.A. = 7h54m26s.45, Decl. = +20 13'04".8 (equinox
1950.0), is superimposed on the nuclear region of a galaxy of mag
18, being roughly 0".6 east and 1".5 south of the galaxy's center.
No such stellar image is present on a technical pan plate (similar
limiting magnitude) obtained in 1990 January, though there is
perhaps a condensation of mag about 20 nearly at the position of
the supernova visible on an old film. A nearby star (mpg = 19) has
end figures 20s.92, 14'17".7.
IAUC 5717
ALPHA ORIONIS (cf E710,E711)
A. K. Dupree, E. Guinan, and M. Smith further report, in addition
to the information on IAUC 5716: "Photometry at Villanova on Feb.
28 UT suggests that alpha Ori has paused in its decline in
brightness at V about +0.9. International Ultraviolet Explorer
observations were acquired as a part of the ongoing monitoring
program on Feb. 24. Radial velocity measurements in the H-alpha
region continue at the McMath Solar Telescope at Kitt Peak."
IAUC 5717
CY URSAE MAJORIS
Taichi Kato, Japan e-mails that he has detected superhumps in
CY UMa during its current outburst (cf E712) and confirms that it
is a new SU UMa-type variable. Further details follow:
Reduction of V-band CCD observations on Mar. 5 yields following
results.
1) Mean magnitude
The star declined from +0.3 to +0.4 in nine hours (comarison: GSC
105705.38 +493730.4 (2000.0) V=12.9). The star may have started
its final decline from the present superoutburst.
2) Detection of superhumps
The hump structures have mean amplitudes of 0.11 mag in V. The
rises are steeper than the declines as in usual superhumps. The
eclipses are not detected.
3) The superhump period
The maxima of superhump occurred at 5.476, 5.546, 5.620, 5.690,
5.763, and 5.838 UT. The times are well expressed by the following
formula:
Max UT = Mar. 5.475 + 0.0723 E
The baseline of the observation was long enough, therefore the
period will be accurate to at least 0.5%.
The period is not in agreement with the previously published one
(Var.Star Bull.) which was based on visual observations only.