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			THE AMERICAN ASSOCIATION OF VARIABLE STAR OBSERVERS 
				25 Birch Street, Cambridge, MA 02138 USA
				BITNET: aavso@cfa	SPAN: cfa::aavso 
				INTERNET: aavso@cfa.harvard.edu 
				Tel. 617-354-0484	FAX 617-354-0665

			AAVSO ALERT NOTICE 181 (March 2,1994)

1844-21 NOVA SAGITTARII 1994

We have been informed b the Central Bureau for Astronomical Telegrams (IAU Circular 
5942) that S. S. Hayashi ~National Astronomical Observatory, Tokyo, Japan) reports that 
Minoru Yamamoto (Okazaki, Aichi, Japan) discovered a nova in Sagittarius on P-MAX 
400 film on February 24.85 UT at photographic magnitude 8.9 and on February 25.84 at 
photographic magnitude 8.5. The object was confirmed by K. Hirosawa (Aichi, Japan), 
who reported the brightness on February 25.85 at visual magnitude 8.5 and provided the 
following position for the nova:

		R.A. 18h 47m 30s	Decl. -21deg 21.0' (1950).

Further magnitude estimates are as follows: Feb. 27.68 UT, 8.53 PEP V (A. Gilmore, Mt. 
John University Observatory, New Zealand), and 27.68, 8.7 (A. Jones, Nelson, New 
Zealand) (via Nova Network); and 28.41, 8.5 (C. Scovil, Stamford; CT); Feb 28.41, 8.4 (J. 
Griese, Stamford, CT); Mar 1.07, 8.0 (D. Overbeek, Edenvale, South Africa); 1.10, 8.0 
(Overbeek).

Accompanying is a finder chart for N Sgr 94 prepared by C. Scovil. Please use this chart to 
observe the nova and telephone your observations to AAVSO Headquarters so we may 
inform the astronomical community. Please indicate which comparison stars you have used 
in making your estimates,

Congratulations to M. Yamamoto on his discovery!

RAPID FADING OF 2337+56 NOVA CASSIOPEIAE 1993

As anticipated (see AAYSO Alert Notice 180), this bright nova has faded rapidly, starting 
with a slow fade from Feb 12 to Feb 15, and since Feb 15 quite rapidly, as indicated by the 
following observations:

Feb 1.00 UT, 8.3 (J. Bortle, Stormville, NY); 1.02, 7.90 PEP V (D. Curott, Florence, AL); 
1.09, 8.0 (R. Royer, Lakewood, CA); 1.09, 8.1 (P. Coffins, Scottsdale, AZ); 1.10, 7.90 PEP V 
(B. Hakes, Peoria, IL); 1.10, 8.29 PEP B (Hakes); 1.90, 8.2 (G. Poyner, Birmingham, 
England); 1.98, 8.1 (F. West, Hanover, PA); 1.99, 8.0 (R. Stewart, Rochelle Park, NJ) ; 
2.04, 8.2 (Poyner); 2.16, 8.4 (Collins); 2.98, 8.2 (West); 3.02, 8.43 PEP V (Curott); 3.05, 8.5 
A. Dill, Wichita, KS); 3.11, 8.4 (D. York, Abiquiu, NM); 3.16, 8.6 (Bortle); 3.17, 8.4 
Collins); 3.79, 8.7 (Poyner); 3.98, 8.3 (G. Gliba, Greenbelt, MD); 4.05, 8.4 (West); 4.07, 8.3 
E. Anderson, Yonkers, NY); 4.78, 8.4 (Po,~ er); 4.81, 8.8 (L. Kiss, Szeged, Hungary); 5.00, 
8.5 West)' ~ 5.07, 8.3 (Anderson)' 5.81, 8.6 tPoYner)' 5.98, 8.5 (Po er)' 6.16, 8.3 (R Royer, 
Lakewood, CA) 6.19, 8.4 (Poyner); 7.00, 8.4 (West); 7.03, 8.3 Anderson); 8.99, 8:5 (G. 
Comello, Groningen, Netherlands); 9.11, 8.1 (Royer); 9.81,8.5 (Comello); 10.04, 8.45 PEP 
V (Hakes); 10.12, 8.5 (Royer); 10.23, 8.3 (P. Schmeer, Bischmisheim, Germany); 10.94, 8.3
(Schmeer); 10.97, 8.3 (S. Sharpe, Bar Harbor, ME); 12.01, 8.6 (Schmeer); 12.03, 8.5 (R. 
Hays, Worth, IL); 12.16, 8.4 (Royer); 12.76, 8.7 (Schmeer); 12.79, 8.6 (Poyner); 13.10, 8.6 
Royer); 14.02, 9.4 (Bortle); 14.02, 9.25 PEP V (Curott); 14.03, 9.0 (Hays); 14.04, 8.8 
(Anderson); 14.13, 8.5 (C. Scovil, Stamford, CT); 14.76, 9.0 (Schmeer); 14.80, 8.9 (L.

Hungary); 14.99, 8.9 (P. Dombrowski, Glastonbury, CT); 14.99, 9.0 (Gliba); 15.05, 9. 
(Anderson); 15.73, 9.2 (Szentasko); 15.75, 10.2 (Kiss); 15.80, 10.1 (M. Moeller, 
Timmendorfer Strand, Germany); 15.80, 9.6 (Tepliczky); 15.87, 9.7 (Szentasko); 15.94, 9.8 
(Comello); 16.03, 10.1 (C. Stephan, Sebring, FL); 16.04, 9.9 (Hays); 16.04, 9.7 (Gliba ; 
16.079 10.1 (Stephan); 16.13, 9.9 (Royer);16.74, 10.2 (Szentasko); 16.78, 10.1 (Schmeer); 
16.82, 10.3 (Szentasko); 16.82, 10.1 (Schmeer); 16.83, 10.1 (Tepliczky); 16.87, 10.1 
Schmeer); 16.91, 10.1 (Schmeer); 16.91,10.2 (Comello);16.94,10.1 Schmeer); 17.00, 10.2 
(Gliba); 17.00, 10.2 (Dombrowski); 17.01, 10.2 (Stewart); 17.03, 10.2 (P. Walker, 
Middlebury, VT); 17.03, 10.15 PEP V (Curott); 17.06, 10.1 (W. Dillon, Missouri City, TX); 
17.12, 10.2 (H. uidry, Littleton, NC); 17.18, 10.1 (E. Broens, Mol, Belgium); 17.23, 10.2 
(T. Vanmunster, Landen, Belgium); 17.23, 10.3 (Schmeer); 17.75, 10.2 (E. Ofek, Tel Aviv, 
Israel); 17.75,10.6 (A. Diepvens, Balen, Belgium); 17.77, 10.5 Vanmunster); 17.77,10.5 
(Vanmunster); 17.77, 10.5 (Broens); 17.80, 10.6 Vanmunster; 17.80, 10.6 (Comello); 
17.84, 10.6 (Vanmunster); 17.85, 10.3 (Schmeer); 17.93, 10.7 (Schmeer); 18.01, 10.5 
Scovil); 18.03, 10.79 PEP V (Curott); 18.06, 10.6 (Dillon); 18.10, 10.6 (Royer ; 18.19, 11.0 
Broens); 18.23, 10.9 (Schmeer); 18.77, 11.1 (Diepvens); 18.78, 11.4 (Schmeer ; 18.78, 11.3 
P. Van Cauteren, Aartselaar, Belgium); 18.82, 11.1 (Broens); 18.83, 11.1 G. Gubbels, 
Tessenderlo, Belgium); 18.84, 11.2 (Comello); 18.85, 11.4 (Schmeer); 18.86, 11.1 
Diepvens); 18.91, 11.4 (Schmeer); 18.93, 11.1 (Broens); 18.93, 11.0 (Gubbels); 19.0, 11.5 
(Dombrowski); 19.00, 11.0 (R. Raphael, S.W. Harbor, ME); 19.00, 11.4 (Sharpe ; 19.03, 
11.5 (Gliba); 19.05, 11.6 (Guidry ; 19.09, 11.3 (Broens); 19.10, 11.2 (Vanmunster); 19.10, 
11.2: (Collins); 19.12,11.4 (Royer); 19.16, 11.1 Broens); 19.18, 11.3 (Diepvens); 19.22, 11.3 
(Diepvens);19.22, 11.4 (Schmeer); 19.22. 11.3 (Vanmunster); 19.78, 11.8 (Schmeer); 19.83, 
11.8 (Schmeer); 19.88, 11.6 (Comello); 20.0, 12.2 (Dombrowski); 20.01, 12.0 (Raphael); 
20.73, 12.6 (N. Stoikidis, Larissa, Greece); 20.78. 12.1 (Diepvens); 20.80, 12.3 (Poyner); 
21.02, 12.4 (M. Adams, Melbourne, FL); 21.10, 12:7 (R. King, Duluth, MN); 21.13, 12.9 
(Royer); 21.20, 12.1 (Vanmunster); 21:94,12.0 (Diepvens); 22.42,12.7 (Dombrowski); 23.0, 
13.3: (Dombrowski); 25.1, 12.3 (York); 25.14, 12.9 CCD UNFILTERED (Royer); 25.99, 
14.2 (Scovil); 25.99, 14.3 (J. Griese, Rocky Hill, CT); 26.00, < 13.8 (Bortle); 27.99, 15.0 
(Griese); 28.0, < 1s.3 (Dombrowski); Mar 1.10, 14.5:, (York); 1.12, < 14.0 (King); 2.13, 14.6 
York).

The optical fading was accompanied by a rapid brightening, followed by a slower increase, 
in the near-infrared, as reported by Kidger et. al. (IAU Circular 5936) and Gamavich (IAU 
Circular 5941), respectively. Shore et. al. (IAU Circular 5934) also report that the 
observations of N Cas 93 with the IUE satellite confirm the formation of dust in the nova 
ejecta during the deep optical decline now underway (IAU Circular 5938).

Once the nova reaches its minimum brightness it should start to brighten slowly, perhaps 
for several months, and then resume its decline, so please keep a very close eye on N Cas 
93 in the coming months. Accompanying is an "e" scale chart prepared by C. Scovil. Please 
use this chart in making observations of N Cas 93 and report your observations to AAVSO 
Headquarters. Please report the comparison stars you used to make your estimates.

Many thanks for your dedicated efforts and valuable astronomical contributions.

Clear skies and good observing!

Janet A. Mattei 
Director

ERRATUM

In AAVSO Alert Notice 180, we reported that N Cas 93 was discovered by Syuichi Nakano. 
In fact, it was discovered by Kazuyoshi Kanatsu and the discovery was reported by Syuichi 
Nakano. We apologize for the error.