High-speed energy-resolved STJ photometry of the eclipsing dwarf nova IY UMa

Abstract

We present high time-resolution photometry of the dwarf nova IY UMa using the S-Cam2 super-conducting tunnel junction device attached to the 4.2m William Herschel Telescope on La Palma. Exploiting the well-defined white dwarf and hot spot eclipse features, we derive an updated orbital ephemeris for IY UMa and an orbital period of 0.07390897(5) days. A white dwarf ingress/egress duration of 31 +/- 2s along with the contact phases of the bright spot gives M_1=0.79 +/- 0.04 M_sun and M_2=0.10 +/- 0.01 Msun, corresponding to a mass ratio of q=0.125 +/- 0.008. The white dwarf eclipse width of 0.0637 then implies i=86.0 +/- 1 degrees. A curious rise with a duration of 30 +/- 2s is observed in the orbital lightcurves during all three observed eclipses. It occurs between the end of white dwarf ingress and hot spot ingress and is blue in colour. We suggest that the source of this light lies in the buried part of the gas stream, resulting in a compact, hot impact cavity.

arXiv comment7 pages, 6 figures, accepted for publication in MNRAS

References in corpus (5)

• The disc instability model of dwarf-novae and low-mass X-ray binary transients
• High-Speed Energy-Resolved STJ Photometry of the Eclipsing Binary UZ For
• Emission line oscillations in the dwarf nova V2051 Ophiuchi
• Late superhumps and the stream-disc impact in IY UMa
• The detection of the donor star in IY UMa

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