THE DYNAMICAL STRUCTURE OF THE
YOUNG REMNANTS OF MASSIVE STAR SUPERNOVAE
The interaction of a massive star supernova with its circumstellar matter
depends on the outer structure of the exploded star and the mass loss from
the progenitor leading up to the supernova. Here we describe a series of
three-dimensional hydrodynamic simulations that we will use to investigate
the structure, dynamics, and emission properties of the young remnants of
massive star supernovae.
Hydrodynamic Models range from idealized self-similar
driven waves to realistic ejecta profiles with embedded clumps evolving into
a nonuniform circumstellar medium.
Numerical Simulations employ an MPI version of
VH-1, an ideal gas dynamics code, on parallel supercomputers to evolve these
SNR models on large 3D grids.
Initial Results
- Self-Similar Driven Waves: We start with the simplest
case of spherically-symmetric ejecta with a power-law density profile evolving
into a smooth circumstellar medium.
- Clumpy Wind: We investigate the effects of a
clumpy progenitor wind on the structure and evolution of SNRs.
- Axisymmetric CSM: We follow up the discovery of a
mechanism by which a small asymmetry in the density of the circumstellar medium
can generate a large protrusion from an otherwise spherical SNR.
Radiative Shocks may be important in determining the
structure and dynamics of the reverse shock in young SNRs. Here we investigate the
stability of a planar radiative shock in two dimensions.