The 2000 Superoutburst of SW UMa

(Superhump light curve by the VSNET SW UMa collaboration team: Makoto Uemura, Taichi Kato, Brian Martin, Rudolf Novak, Denis Buczynski, Lew Cook, Elena Pavlenko, Sergei Shugarov, Nataly Katisheva, Gianluca Masi, Alessia Cassetti, Kohji Yoshikawa)

(Superhump light curve by the VSNET SW UMa collaboration team)

(Regrowth of superhumps on Feb. 27, observation by the Kyoto team and Rudolf Novak)

(Prominent superhumps and super(?)-QPOs seen during the final decline)

Successful international collaboration ongoing!

(vsnet-alert 4185)

Dear colleagues,

  SW UMa is entering outburst:

UMASW        000211.927  15.0   KNN
UMASW        000211.953  14.2   KNN

(RX J0909.8+1849 was detected at 14.2)
Timo Kinnunen

(vsnet-alert 4186)

Positive observations of SW UMa

Mr C. P. Jones
Laindon, Essex, UK.

Instrument: 457mm f/4 Newtonian + 150mm and 75mm masks.

Visual Observations for 11 February 2000.

11 Feb  Transparent.

Star            UT                  Mag              Seq  Comments
UMASW           000211.9257         14.1     JCN     BAA  Outburst!
UMASW           000211.9549         14.1     JCN     BAA

Chris J 

(vsnet-alert 4188)

Visual magnitude estimates by P. Schmeer, Bischmisheim, Germany:

Feb. 11.23  UT, [13.0 ; 11.77 , [13.2 ; 12.028,  12.4 ; 12.062,  12.0 ;
     12.085 UT,  11.7
Sequence:   AAVSO
Instrument: 203-mm SCT
Going into outburst just between my evening and midnight session - great!
The most recently recorded outburst (a supermaximum) was detected by Gene
Hanson on 1997 Oct. 19.490 UT at mv= 11.1 (cf. vsnet-alert 1269, IAUC 6760).

(vsnet-alert 4194)

SW UMa outburst confirmed

Dear Colleagues,

We have just confirmed the rare outburst of SW UMa. The object has been observed at around mag 11. The present brightness may be indicative that the object is on the premaximum halt (or precursor) to the final rise, or that the present outburst can be either faint superoutburst or a normal outburst. The interval exceeding two years since the latest superoutburst may more prefer the first interpretation. Observations are very strongly encouraged.

Taichi Kato and Makoto Uemura

(vsnet-alert 4201)

SW UMa: brightening and international campaign

Our CCD observation has confirmed the further ongoing brightening of SW UMa. The object has become 0.4 mag brighter in these 4 hours. This may reflect the final rise to the peak brightness! We presently use 10 sec exposure time in order to resolve possible super-QPOs.

We will undertake an international observing campaign on SW UMa, as we have had a very successful one in DV UMa and IY UMa. Please post timely to vsnet-alert confirmatory observations, new findings, the progress of the outburst and observations. Collaborating observations should be sent (as usual) to

Makoto Uemura and Taichi Kato

(vsnet-alert 4209)

SW UMa was rapidly brightening with a rate of 0.6 mag/d during our last night run for 10 hours (some clouds and other target made our light curve sparse). We cannot see superhump and super-QPO in the light curve, but the modulation with the amplitude of 0.05mag is seen.

We are now observing SW UMa with exposure-time of 10s, but the weather is not good, so other site observations are strongly encouraged.

Makoto Uemura and Taichi Kato

(vsnet-alert 4228)

From last night observation on SW UMa at Kyoto, we detected a modulation with the amplitude of over 0.1mag while fully evolved superhump is still not seen. Compared with the other superoutburst of SU UMa stars, the appearance of the definite superhump is relatively late.

Makoto Uemura and Taichi Kato

(vsnet-alert 4244)

SW UMa: superhump evolved

In the light curve of SW UMa on Feb. 16 observed at Kyoto, we see the evolution of the superhump whose amplitude varied from about 0.1 mag to 0.2 mag within 10 hours. The following observation by B. Martin showed the 7 superhumps with almost constant amplitude of 0.2 mag. The observations are urged to catch the more evolutional scenario of superhump.

Makoto Uemura, Taichi Kato and Brian Martin

VSNET light curve (requires Java)

Light curve

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