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

Bąkowska K., Olech A.

Acta Astronomica

2015

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.

Disk Eclipse in IY UMa: Further Evidence for Stream Overflow

Smak J.

Acta Astronomica

2003

Vol. 56, No. 2

167--173

Disk eclipse light curve of dwarf nova IY UMa at quiescence (Steeghs et al. 2003) is analyzed. It is found that about 10% of the observed disk flux comes from parts of the stream which are overflowing the disk. They are also responsible for the residual flickering present during total eclipse of the hot spot. The fraction of mass involved in the stream overflow is very crudely estimated to be about 20%.