Mirror eclipses in the dwarf nova IP Peg

Details Mirror eclipses in the dwarf nova IP Peg Mirror eclipses in the dwarf nova IP Peg

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aspc..261..499l&link_type=abstract

The Physics of Cataclysmic Variables and Related Objects, ASP Conference Proceedings, Vol. 261. Edited by B. T. Gänsicke, K. Beu

Physics

Scientific paper

Recent time-resolved K band spectroscopy of the dwarf nova IP Pegasi shows a unique feature centred around phase 0.5. At first viewing the feature appears to be a unusual eclipse of the disc light, in which the classic rotational disturbance is reversed. This feature is interpreted as the partial absorption of secondary star light at emission line wavelengths by a translucent accretion disc. The implication, that the bulk of the accretion disc is optically thin at continuum wavelengths, has important ramifications for disc instability models of dwarf nova outbursts. The details of this work are published in Littlefair et al. (2001).

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