THE AMERICAN ASSOCIATION OF VARIABLE STAR OBSERVERS
25 Birch Street, Cambridge, MA 02138 USA
BITNET: aavso@cfa SPAN: cfa::aavso
INTERNET: firstname.lastname@example.org 
Tel. 617-354-0484 FAX 617-354-0665
AAVSO ALERT NOTICE 193 (September 29, 1994)
OUTBURST OF CATACLYSMIC VARIABLE 2325+43 DX ANDROMEDAE
We have been informed by Tonny Vanmunster, Landen, Belgium (Belgian
Astronomical Society, VVS, Cataclysmic Variable Circular (CVC) 17), Guy Hurst,
Basingstoke, England, (The Astronomer (TA) E886), and AAVSO observers in the
United States that the dwarf nova type cataclysmic variable DX And is
undergoing an outburst, as indicated by the following observations:
Sep 23.833 UT, 12.6, T. Vanmunster, Landen, Belgium (via CVC); 23.872, 12.3,
J. Pietz, Erftstadts, Germany (via CVC); 24.810, 12.2, M. Westlund, Uppsala,
Sweden (via TA); 27.067, 11.7, J. Nordby, Moorhead, MN; 28.081, 11.8, R.
Stewart, Rochelle Park, NJ; 28.195, 11.6, J. McKenna, Upper Montclair, NJ;
29.127, 11.6, Stewart; 29.211, 12.1, McKenna; 29.300, 12.1, Nordby; 29.375,
12.0, W. Albrecht, Pahala, HI.
The most recent outbursts of this cataclysmic variable occurred in August
1993, when DX And reached magnitude 10.7 at maximum (Tonny Vanmunster was the
first observer to detect the start of this outburst), and in February 1992,
when it reached magnitude 11.6. The outbursts generally last two to three
Please monitor the current outburst of DX And closely, using the accompanying
finder chart, and report your observations to AAVSO Headquarters.
Chart links are obsolete; 01/2014 create charts using VSP at http://www.aavso.org/vsp 
2027+52 V1974 CYGNI = NOVA CYGNI 1992
We have been informed via VSNET in Japan that Brian Skiff, Lowell Observatory,
has provided faint photoelectric magnitudes for the field of N Cyg 92 = V1974
Cyg. These magnitudes are for the comparison stars marked 13.4 and 14.5 on
the accompanying finder chart. The 13.4 was measured by Skiff last year at
V=13.42; we have kept the magnitude at 13.4 for homogeneity of observations.
The 145 extends the sequence photoelectrically. Also, early in 1994, Charles
Scovil obtained a photovisual sequence by measuring the plates of V1974 Cyg;
his photovisual sequence was not widely distributed at the time, but is
incorporated into the accompanying chart. We welcome comments from observers
as to how the 14.2 photovisual, 14.5 photoelectric, and 15.0 photovisual fit
together, and also how they match the brighter end of the sequence. It is
interesting and encouraging to note that Scovil obtained the same photovisual
magnitude (i.e., 14.5) for the 14.5 comparison star that Skiff measured
photoelectrically. Please indicate the comparison stars you used when making
brightness estimates of V1974 Cyg.
REQUEST TO MONITOR CATACLYSMIC VARIABLES FOR THE HUBBLE SPACE TELESCOPE (HST) AND INTERNATIONAL ULTRAVIOLET EXPLORER (IUE)
Please monitor the following cataclysmic variables that will be in the
observing program of HST in October:
Desig Name Type Present brightness Scheduled observation
0201+14 TT Ari Dwarf nova 10.5 Oct 7 11:00 - 17:44 UT
2318+17 IP Peg Dwarf nova 11.8 - 15.3-15.8 Oct 8 13:50 - 16:20 UT
2318+17 IP Peg Oct 9 01:05 - 03:38 UT
1843+00 V603 Aql Nova 1918 11.4 Oct 12 05:00 - 11:30 UT
We have a standing request from astronomers at the VILSPA Station of the IUE
in Spain to be alerted to activity in the stars described below, as they plan
to observe these objects with the IUE when the circumstances are appropriate:
2138+43 SS CYGNI. Please notify us of the outburst of SS Cyg in case the
outburst should be an anomalous one, that is, a symmetrical outburst in which
the rise is slow.
1813+49 AM HERCULIS. Please monitor this cataclysmic variable closely
whenever possible and call your observations in to AAVSO Headquarters when it
begins to fade to its down state.
OUTBURST OF 1439+22A UZ BOOTIS
Our sincere thanks to those observers who monitored the recent rare outburst
of UZ Boo. An interesting feature of the outburst was that immediately after
the star faded, it briefly brightened again. Presently, we are studying the
outburst behavior of UZ Boo, including this unusual behavior. Checking our
database, we find that brightening right after outburst is not unprecedented
for UZ Boo - there is an observation made by C. Scovil of the 1978 outburst
which indicates that the star may have brightened immediately after it faded.
UPDATES ON A FEW SOUTHERN R CORONAE BOREALIS TYPE VARIABLES
Danie Overbeek, Edenvale, South Africa, informs us that the following Southern
hemisphere R CrB stars are fading:
1834-23 V348 SAGITTARII - Aug 29.8 UT, 13.2; 30.7, 13.2; 31.7, 13.3;
Sep 1.7, 13.2; 2.7, 13.2; 3.7, 13.2; 4.7, <13.4; 5.7, <13.1; 6.7, <13.4;
7.7, <13.4; 9.7, <13.4.
1428-39 V854 CENTAURI - Aug 30.7 UT, 10.2; 31.7, 10.6; Sep 1.7, 10.8;
2.7, 11.4; 3.7, 12.0; 4.7, 12.7; 5.7, 12.8; 6.7, 12.9; 7.7, <13.0; 9.7, <13.0.
D. Overbeek also informs us that RZ Nor, which had been at maximum at around
magnitude 11 until September 11, has also started to fade, and provides us
with the following observations: Sep 11.7 UT, 11.2; 14.7, 11.8; 15.7, 12.0;
16.7, 12.3; 18.7, 12.5; 19.7, 12.7.
OUTBURST OF 2209+12 RU PEGASI
We have just been informed that the dwarf nova cataclysmic variable RU Peg
is in outburst. Most recently, RU Peg has had two faint outbursts, one in
May 1994 when it reached magnitude 11.4, and one in June 1994 when it reached
magnitude 11.6. Current observations include: Sep 29.153 UT, 11.4, W. Dillon,
Missouri City, TX; 29.205, 11.2, J. McKenna, Upper Montclair, NJ; 29.370,
11.8, W. Albrecht, Pahala, HI.
The answering machine at Headquarters, with our charge free number
(1-800-642-3883), is on nights and weekends for your convenience.
Many thanks for your dedicated efforts and valuable observations.
Janet A. Mattei
SUBMIT OBSERVATIONS TO THE AAVSO
Information on submitting observations to the AAVSO may be found at:
ALERT NOTICE ARCHIVE AND SUBSCRIPTION INFORMATION
An Alert Notice archive is available at the following URL:
Subscribing and Unsubscribing may be done at the following URL:
Please support the AAVSO and its mission -- Join or donate today: