Onset of Convectionon a Pre-Runaway White Dwarf

Details Onset of Convectionon a Pre-Runaway White Dwarf Onset of Convectionon a Pre-Runaway White Dwarf

2002-07-26

arxiv.org/abs/astro-ph/0207595v1

AIP Conf.Proc. 637 (2003) 139-143

Astronomy and Astrophysics

Astrophysics

5 pages, 4 figures, from the 2002 International Conference on Classical Novae in Sitges, Spain

Scientific paper

10.1063/1.1518191

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.

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