  Observed novae abundances and explosion energies estimated from observations
indicate that there must be significant mixing of the heavier material of the
white dwarf (C+O) into the lighter accreted material (H+He). Accordingly, nova
models must incorporate a mechanism that will dredge up the heavier white dwarf
material, and fluid motions from an early convection phase is one proposed
mechanism.
  We present results from two-dimensional simulations of classical nova
precursor models that demonstrate the beginning of a convective phase during
the `simmering' of a Nova precursor. We use a new hydrostatic equilibrium
hydrodynamics module recently developed for the adaptive-mesh code FLASH. The
two-dimensional models are based on the one-dimensional models of Ami Glasner,
and were evolved with FLASH from a pre-convective state to the onset of
convection.

Astrophysics