1994A&A...288..175M

We study the structure of a corona above a dwarf nova accretion disk. The interaction between the cool disk and the hot corona is investigated with a one-zone model. The result is that a siphon flow evaporates the corona. The material partially accretes through the coronal layers on to the white dwarf, partially is lost via a wind. Consequences are a hole in the inner accretion disk near the white dwarf and therefore a retarded change of the disk to the hot state in the beginning of an outburst. This shows up as a delay of the UV radiation.