Structure and properties of transition fronts in accretion discs

We use high‐resolution time‐dependent numerical simulations of accretion discs around white dwarfs to study the structure and properties of transition fronts in the context of the thermal‐‐viscous disc instability model. The thermal structure of cooling and heating fronts is dominated by radiative cooling and viscous heating, respectively, except in a very narrow precursor region in heating fronts where advection and radial transport of energy dominate. Cooling fronts are much broader than heating fronts, but the widths of both types of fronts scale with the local vertical scaleheight of the disc. We confirm that during a fair fraction of the propagation time of a cooling front, the structure of the inner disc is close to self‐similar. The speed of heating fronts is ∼ a few km s ‐1 , while the speed of cooling fronts is ∼ a fraction of a km s ‐1 . We show that direct measurements of the speed of transition fronts probably cannot discriminate between various prescriptions proposed for the viscosity parameter α. A natural prediction of the disc instability model is that fronts decelerate as they propagate in the disc, independent of the prescription for α. Observation of this effect would confirm that dwarf nova outbursts are driven by the thermal‐‐viscous instability. Most of our results also apply to low‐mass X‐ray binaries in which the accreting object is a neutron star or a black hole.