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Hot Spot Manifestation in Eclipsing Dwarf Nova HT Cassiopeiae

100%

Bąkowska K. , Olech A.

Acta Astronomica

2014

tom Vol. 64, No. 3

247--259

We report the detection of a hot spot in the light curves of the eclipsing dwarf nova HT Cas during its superoutburst in 2010 November. Analysis of the eight reconstructed light curves of the hot spot eclipses showed directly that the brightness of the hot spot was changing significantly during the superoutburst. Thereby, detected hot spot manifestation in HT Cas is the newest observational evidence for the EMT model for dwarf novae.

Hot Spot in Eclipsing Dwarf Nova IY Ursae Majoris during Quiescence and Normal Outburst

100%

Bąkowska K. , Olech A.

2015

tom Vol. 65, No. 4

351--360

We present the analysis of hot spot brightness in light curves of the eclipsing dwarf nova IY UMa during its normal outburst in March 2013 and in quiescence in April 2012 and in October 2015. Examination of four reconstructed light curves of the hot spot eclipses showed directly that the brightness of the hot spot changed significantly only during the outburst. The brightness of the hot spot, before and after the outburst, was on the same level. Thus, based on the behavior of the hot spot, IY UMa during its normal outburst follows the disk-instability model.

The 2003 and 2005 Superhumps in V1113 Cygni

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Bąkowska K. , Olech A. , Złoczewski K. , Wiśniewski M.

Acta Astronomica

2010

tom Vol. 60, No. 2

137--147

We report CCD photometry of the cataclysmic variable star V1113 Cyg. During two campaigns, lasting from May to August 2003 and from March to June 2005, we recorded two superoutbursts. In the obtained light curves we detected clear superhumps with a mean period Psh=0.07891(3) days (113.63±0.04 min). That fact confirms that the star is a member of SU UMa class of dwarf novae. During the first observed superoutburst the superhump period was decreasing with an enormous rate of P=-4.5(8)×10-4 which is one of the highest values ever observed in SU UMa systems.

CzeV404 - an Eclipsing Dwarf Nova in the Period Gap During its July 2014 Superoutburst

70%

Bąkowska K. , Olech A. , Pospieszyński R. , Martinelli F. , Marciniak A.

Acta Astronomica

2014

tom Vol. 64, No. 4

337--348

Results of the CCD observations of CzeV404 are presented. During the season of June-August 2014 we detected one outburst and one superoutburst of the star. Clear superhumps with the period of Psh=0.10472(2) days were observed. The superhump period was decreasing with a high value of dP/dt=-2.43(8)×10-4. From 17 eclipses we calculated the orbital period with the value of Porb=0.0980203(6) days which confirms that CzeV404 belongs to period gap objects and it is the longest orbital period of an eclipsing SU UMa star. Based on superhump and orbital period determinations, the period excess ε=6.8%±0.02% and the mass ratio q≈0.32; of the system were obtained.

New Photometric and Spectroscopic Observations of the Eclipsing Binary V2080 Cygni

51%

Dimitrov W. , Kamiński K. , Bąkowska K. , Kamińska M. K. , Tokarek J. , Pawłowski M. , Boneva D. , Bartczak P. , Kwiatkowski T. , Schwarzenberg-Czerny A.

Acta Astronomica

2022

tom Vol. 72, No. 1

55--67

We present new spectroscopic and photometric measurements of the eclipsing binary V2080 Cyg. It is a detached system with similar components and an orbital period of 4.9 d. We collected spectroscopic data with two instruments, 1.88 m DDO telescope equipped with Cassegrain spectrograph and 0.5 m PST1 connected to a fiber-fed echell\'e spectrograph. We collected 127 measurements for each component, which significantly increase the number of available radial velocity measurements for the V2080 Cyg system. Obtained masses of the eclipsing components are M1=1.189± 0.007 and M2=1.138±0.007 M☉. We also collected a multicolor photometry. The three-band light curves obtained together with the radial velocity data enabled us to calculate the model of the system. New estimations of the orbital inclination and radii of the components were computed. We obtained as well new times of minima. The O-C diagrams indicate variation, which requires more recent data to be confirmed. The possible existence of a third body could cause a light-time effect in the system. In addition, we analyze the Gaia mission results. V2080 Cyg A has three visual companions. However, according to Gaia parallaxes and proper motions, they cannot be dynamically connected with the eclipsing binary and therefore are background stars.