Volume 452, Number 3, June IV 2006
|Page(s)||933 - 939|
|Section||Stellar structure and evolution|
|Published online||06 June 2006|
The CUrious Variables Experiment (CURVE). Variable properties of the dwarf nova SS Ursae Minoris
Nicolaus Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warszawa, Poland e-mail: olech,firstname.lastname@example.org
2 Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland e-mail: [kmularcz;pkedzier;kzlocz]@astrouw.edu.pl
Accepted: 18 January 2006
We report on extensive photometry of the dwarf nova SS Ursae Minoris throughout nine months of 2004. In total, we recorded two superoutbursts and 11 normal outbursts of the star. SS UMi has been known to show frequent superoutbursts with a mean interval of 84.7 days. Our data suggest that the interval between successive superoutbursts lengthened to 197 days, indicating that SS UMi entered a period of untypical behavior manifested by a growth in the quiescent magnitude of the star and a series of frequent, low-amplitude, normal outbursts observed from July to September 2004. The mean superhump period derived for the April 2004 superoutburst of SS UMi is days ( min). Combining this value with an earlier orbital period determination, we were able to derive the period excess, which is equal to %, and estimate the mass ratio of the binary system as equal to . During the entire superoutburst, the period decreased at a rate of . However, detailed analysis of the timings of superhump maxima seem to suggest a more complex period change, with a decrease in the period during the first and last stages of the superoutburst but an increase in the middle interval.
Key words: stars: binaries: close / stars: variables: general / stars: dwarf novae
© ESO, 2006
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