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Accretion Disk Winds in Cataclysmic Variables

Published online by Cambridge University Press:  12 April 2016

Christian Knigge,
Janet E. Drew and
Keith O. Mason
Christian Knigge
Affiliation:
Nucl. & Astroph. Lab., Keble Road, Oxford, OX1 3RH, UK
Janet E. Drew
Affiliation:
Nucl. & Astroph. Lab., Keble Road, Oxford, OX1 3RH, UK
Keith O. Mason
Affiliation:
Mullard Spa. Sci. Lab., Surrey, RH5 6NT, UK

Abstract

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We present preliminary results of a modelling campaign based on HST eclipse observations of the wind-formed C IV resonance line in the eclipsing nova-like variable UX UMa. Within the framework of a simple kinematic accretion disk wind model, we are currently able to reproduce the shapes (but not the strengths) of the observed line profiles away from and during eclipse, as well as the behaviour of the integrated line flux light curve. The most important aspect of our modelling is that it suggests the presence of a vertically extended, relatively dense and slow moving transition region between the disk photosphere and the fast wind.

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