THE ASTRONOMER Electronic Circular No 707       1993 Feb 17 22.11UT
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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SW URSAE MAJORIS
Bjorn Granslo, Oslo, Norway reports his detection of an outburst of
this dwarf nova. Confirmation has subsequently been obtained by
Haakon Dahle, Oslo, Norway and Ornulf Midtskogen, Tranby, Norway:
1993 Feb 16.13UT, [13.5 Class 1 B.Granslo    C203 x123
	 17.111    10.9       1 B.Granslo    C203 x123
	 17.743    11.2         H.Dahle      C203 x123
	 17.762    11.0         O.Midtskogen M316, x62
Granslo adds:
"High-speed photometry is required during the current outburst in
order to detect superhumps, quasi-periodic oscillations and other
short-periodic phenomena. The last outbursts started on 1991
February 25 and 1992 March 19."

Taichi Kato, Japan e-mails further notes:
"According to the alert from B. H. Granslo, the dwarf nova SW UMa
is currently in outburst.
During the preceding outburst (Mar, 1992), "super-quasi-periodic-
oscillations" (super-QPOs) with an amplitude of 0.2 mag and a
period of 6.1 min was detected  (T.Kato et al., 1992, Publ. Astron.
Soc. Japan, L215-L219). The QPOs showed sharp eclipse-like dips
with a duration of one minute and we suggest that super-QPOs may
originate from the eclipse of the central object by an orbiting
blob or the inflation of the accretion disk.  Such phenomena of
gigantic amplitudes (nearly equal to the amplitude of superhumps)
can be detected by visual observations, so we would like to urge
visual observers to monitor this star throughout the outburst with
time-resolution as short as possible (at least 1 min).

IP PEGASI
Further to the note on E706 of an outburst of this star, Taichi
Kato provides further information:

IP Pegasi (V-band)
       UT         V-C
   Feb. 3.3863   +1.86 *1
	3.3871   +2.20 *1
   Feb. 5.3830   +3.20
	5.3837   +3.26
	5.3845   +3.20
	5.3852   +3.05
	5.3858   +3.01
  V = IP Peg
  C = 232311.01 +182513.7 (2000.0) 10.8
  (*1 scatter due to string twilight)

The mean mangitudes of IP Peg were V=12.8 on Feb. 2 and V=13.9 on
Feb. 5.

NGC 4151
Further to the note on E699, Taichi Kato provides further
information:
NGC4151 (V-band)
	UT         V-C1
   Feb. 2.814     +1.79 +/- 0.01 (3 frames)
   Feb. 5.650     +1.76
	5.651     +1.76
	5.652     +1.76
  C1: BD+40.2507  V=9.83 B-V=0.59 U-B=-0.01