UC Santa Barbara

Thermonuclear burning of hydrogen on white dwarfs (WDs) is an inevitable occurence for accreting WDs in binary systems. After the onset of thermally-unstable nuclear burning, the WD rapidly expands and ejects much of its hydrogen-rich matter. Once it regains thermal equilibrium, it contracts and becomes a luminous source of supersoft X-rays. This supersoft phase can last anywhere from days (for novae on massive WDs) to millions of years (for persistent supersoft sources). In this dissertation, we explore how the supersoft phase of accreting WDs proceeds and what observations of it reveal about the underlying WD. We present stellar models of persistent supersoft sources and novae. We then use these models to explain the isothermal nature of the ejecta as observed in the radio. We also use these models to test the efficacy of g-modes excited in the burning layer as an explanation of observed oscillations in the supersoft phase of novae. While we find excited modes, their periods are too short to account for the observed oscillations.