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Summary: Active Carbon and Oxygen Shell Burning Hydrodynamics
Casey A. Meakin1
& David Arnett1
cmeakin@as.arizona.edu, darnett@as.arizona.edu
ABSTRACT
We have simulated 2.5×103
seconds of the late evolution of a 23M star
with full hydrodynamic behavior. We present the first simulations of a multiple-
shell burning epoch, including the concurrent evolution and interaction of an
oxygen and carbon burning shell. In addition, we have evolved a 3D model
of the oxygen burning shell to sufficiently long times (300 seconds) to begin
to assess the adequacy of the 2D approximation. We summarize striking new
results: (1) strong interactions occur between active carbon and oxygen burning
shells, (2) hydrodynamic wave motions in nonconvective regions, generated at
the convective-radiative boundaries, are energetically important in both 2D and
3D with important consequences for compositional mixing, and (3) a spectrum of
mixed p- and g-modes are unambiguously identified with corresponding adiabatic
waves in these computational domains. We find that 2D convective motions are
exaggerated relative to 3D because of vortex instability in 3D. We discuss the
implications for supernova progenitor evolution and symmetry breaking in core
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