Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aipc..565...81h&link_type=abstract
YOUNG SUPERNOVA REMNANTS: Eleventh Astrophysics Conference. AIP Conference Proceedings, Volume 565, pp. 81-84 (2001).
Astronomy and Astrophysics
Astrophysics
Supernova Remnants, Pre-Main Sequence Objects, Young Stellar Objects And Protostars, Mass Loss And Stellar Winds
Scientific paper
The interaction of a young supernova remnant and its surroundings can be described by a self-similar solution if the expanding supernova ejecta can be described by a power law density profile of ρ~r-n with n>5, and the surrounding ambient medium has a density power law of ρ~r-s with s<3 [1]. It has been shown in two dimensions that initializing a hydrodynamics code with the self-similar solution for the interaction region and perturbing the density randomly causes Rayleigh-Taylor instabilities [2]. We present hydrodynamic simulations of self-similar driven waves, with different parameters, for the purpose of comparing the growth and saturation of the convective instability in three dimensions compared to two dimensions. The contact discontinuity in all simulations produced Rayleigh-Taylor fingers with predictable morphologies; long, continually growing spikes for s=2, and shorter, mushroom capped blobs for s=0. A fourier spectrum was obtained and compared in both two and three dimensions to analyze the evolution of the instability's growth. Turbulent energy density was measured and compared for different initial conditions. These simulations and diagnostics show how closely two-dimension codes can approximate three-dimensions and also provide information on expansion and mixing of young supernova remnants. .
Blondin John M.
Hinkle Christopher L.
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