Wyniki wyszukiwania - BazTech

Ograniczanie wyników

2 Acta Astronomica

Powiadomienia systemowe

Sesja wygasła!

Znaleziono wyników: 2

Liczba wyników na stronie

Wyniki wyszukiwania

Sortuj według:

Ogranicz wyniki do:

2009 Superoutburst of Dwarf Nova 1RXS J053234.9+624755

Rutkowski A., Olech A., Poleski R., Sobolewska M., Kankiewicz P., Ak T., Boyd D.

Acta Astronomica

2010

Vol. 60, No. 4

337--355

We present photometric observations of the dwarf nova 1RXS J053234.9+624755. We performed a detailed analysis of the superoutburst that occurred in August 2009. We found the superhump period to be Psh=0.057122(14) days. Based on the O-C diagram we conclude that Psh increased during the plateau at the rate of dPsh/dt=(9.24±1.4)×10-5. Both the O-C analysis and evolution of the superhumps light curve favor the model in which superhumps originate in a variable source located in the vicinity of the hot spot. In addition, the evolution of the light curve suggests that the superhump light source approaches the disk plane as the superoutburst declines. Detailed analysis of the superoutburst plateau phase enabled us to detect a signal which we interpret as apsidal motion of the accretion disk. We detected additional modulations during the final stage of the superoutburst characterized by periods of 104 s and 188 s which we tentatively interpret as quasi periodic oscillations. Estimations of A0 and An are in agreement with the dependence between the amplitude of superhumps and the orbital inclination.

Curious Variables Experiment (CURVE). CCD Photometry of V419 Lyr in its 2006 July Superoutburst

Rutkowski A., Olech A., Mularczyk K., Boyd D., Koff R., Wiśniewski M.

Acta Astronomica

2007

Vol. 57, No. 3

267--279

We report extensive photometry of the dwarf nova V419 Lyr throughout its 2006 July superoutburst till quiescence. The superoutburst with amplitude of ≈3.5 mag lasted at least 15 days and was characterized by the presence of clear superhumps with a mean period of Psh=0.089985(58) days (129.58±0.08 min). According to the Stolz-Schoembs relation, this indicates that the orbital period of the binary should be around 0.086 days i.e., within the period gap. During the superoutburst the superhump period was decreasing with the rate of P/Psh=-24.8(2.2)×10-5, which is one of the highest values ever observed in SU UMa systems. At the end of the plateau phase, the superhump period stabilized at a value of 0.08983(8) days. The superhump amplitude decreased from 0.3 mag at the beginning of the superoutburst to 0.1 mag at its end. In the case of V419 Lyr we have not observed clear secondary humps, which seems to be typical for long period systems.