Dwarf novae in outburst: modelling the observations

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Abstract
We construct time-dependent accretion-disc models and use them to calculate theoretical spectra in order to try to fit the ultraviolet and optical observations of outbursts of the two dwarf novae VW Hydri and CN Orionis. We find that the behaviour on the rise to outburst is the strongest discriminator between theoretical models. The mass-transfer burst model is able to fit the spectral behaviour for both objects. The disc-instability model is unable to fit the rise to outburst in VW Hydri, and gives a poor fit to the observations of CN Orionis. We discuss the accuracy of the modelling procedures we have adopted and how they might be improved and comment on the implications of our findings.

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