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We explore the consequences of a magnetic dynamo origin for the viscosity inaccretion discs, for the structure and evolution of discs in dwarf novasystems. We propose that the rapid cooling that sets in at the end of a dwarfnova eruption acts to inhibit the Balbus-Hawley instability, and thereby toquench dynamo action and so reduce disc viscosity. We demonstrate that amodified disc instability model can reproduce the basic properties of dwarfnova eruptions, as well as some properties of quiescent discs. We also discusssome observational consequences of our model.Comment: uu-encoded gz-compressed Postscript file, 18 pages including 6  figures. ApJ in pres

Dynamo Driven Accretion Discs and Dwarf Nova Eruptions