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Title:
High-speed energy-resolved STJ photometry of the eclipsing dwarf nova IY UMa
Authors:
Steeghs, D.; Perryman, M. A. C.; Reynolds, A.; de Bruijne, J. H. J.; Marsh, T.; Dhillon, V. S.; Peacock, A.
Affiliation:
AA(Department of Physics and Astronomy, University of Southampton, Highfield, Southampton S017 1BJ), AB(Astrophysics Missions Division, Research and Scientific Support Department, ESTEC, PO Box 299, 2200 AG Noordwijk, the Netherlands), AC(Astrophysics Missions Division, Research and Scientific Support Department, ESTEC, PO Box 299, 2200 AG Noordwijk, the Netherlands), AD(Astrophysics Missions Division, Research and Scientific Support Department, ESTEC, PO Box 299, 2200 AG Noordwijk, the Netherlands), AE(Department of Physics and Astronomy, University of Southampton, Highfield, Southampton S017 1BJ), AF(Department of Physics and Astronomy, University of Sheffield, Sheffield S3 7RH), AG(Astrophysics Missions Division, Research and Scientific Support Department, ESTEC, PO Box 299, 2200 AG Noordwijk, the Netherlands)
Publication:
Monthly Notice of the Royal Astronomical Society, Volume 339, Issue 3, pp. 810-816. (MNRAS Homepage)
Publication Date:
03/2003
Origin:
MNRAS
MNRAS Keywords:
accretion, accretion discs, binaries: eclipsing, stars: dwarf novae, stars: individual: IY UMa, novae, cataclysmic variables
DOI:
10.1046/j.1365-8711.2003.06226.x
Bibliographic Code:
2003MNRAS.339..810S

Abstract

We present high-time-resolution photometry of the dwarf nova IY UMa using the S-Cam2 superconducting tunnel junction device attached to the 4.2-m William Herschel Telescope on La Palma. Exploiting the well-defined white dwarf and hotspot eclipse features, we derive an updated orbital ephemeris for IY UMa and an orbital period of 0.07390897(5) d. A white dwarf ingress/egress duration of 31 ± 2 s along with the contact phases of the bright-spot gives M1= 0.79 ± 0.04 Msolar and M2= 0.10 ± 0.01 Msolar, corresponding to a mass ratio of q= 0.125 ± 0.008. The white dwarf eclipse width of ΔφWD= 0.0637 then implies . A curious rise with a duration of 30 ± 2 s is present in the orbital light curves during all three observed eclipses. It occurs between the end of white dwarf ingress and hotspot 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.

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