Convection and Mixing in Classical Novae Precursors

Details Convection and Mixing in Classical Novae Precursors Convection and Mixing in Classical Novae Precursors

Jun 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...200.9502d&link_type=abstract

American Astronomical Society, 200th AAS Meeting, #95.02; Bulletin of the American Astronomical Society, Vol. 34, p.955

Astronomy and Astrophysics

Astronomy

Scientific paper

To explain observed abundances from classical nova outbursts, and to help explain their energetics, nova models must incorporate a mechanism that will dredge up the heavier white dwarf material into the lighter accreted atmosphere. One proposed mechanism relies on the fluid motions from an early convective phase to do the mixing. We present recent work investigating two aspects of this mechanism. We examine 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 (Glasner et al. 1997), and were evolved with FLASH from a pre-convective state to the onset of convection. The onset of convection induces a velocity field near the C,O/H,He interface, which can then cause mixing through interactions with gravity waves. We show results from simulations of these wind-wave interactions, and estimate whether the `wind' caused by the convection could induce sufficient dredge-up to power a classical novae. This research has been supported by the US. Department of Energy under grant no. B341495 to the ASCI Flash Center at the University of Chicago

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