Computer Science – Sound
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21743320n&link_type=abstract
American Astronomical Society, AAS Meeting #217, #433.20; Bulletin of the American Astronomical Society, Vol. 43, 2011
Computer Science
Sound
Scientific paper
Using ENZO, a cosmological adaptive mesh refinement (AMR) code, and YT, a python package used to analyze AMR data, we run simulations of shockwave propagation through a variously characterized medium at high-resolutions. The characteristics of the shock itself are similarly varied. We then analyze the dependence of microstructure formation in the propagating shock on conditions of velocity, density, temperature, and metallicity of both the shock and medium. Advancing the simulation, we allow the instabilities to develop to some derived time based on initial conditions. We find strong correlations between particle density, temperature, and metallicity in determining the features of the shock column, the development of thick or thin `fingers', and the distribution of energy, metals, and propagated material. We found the most interesting results when using temperatures in the range of 1,000K to 10,000K, shock velocities of 2 to 8 times the sound speed, densities of 10 to 100 particles per cubic centimeter, and metallicities of 0 to 2.2e-4, with analytic comparisons of parameter sets with and without a metal cooling mechanism, however we do maintain radiative cooling. We examine the significance of these results and what they may suggest in discussions of material propagation between generations of stars. Implications of interstellar enrichment are also considered.
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