Simulations of Supernova Reverse Shock Dust Destruction in Metal-Enriched Clouds

Details Simulations of Supernova Reverse Shock Dust Destruction in Metal-Enriched Clouds Simulations of Supernova Reverse Shock Dust Destruction in Metal-Enriched Clouds

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21725620s&link_type=abstract

American Astronomical Society, AAS Meeting #217, #256.20; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

In following previous work, we present hydrodynamic simulations used to study the effects of dust destruction by sputtering in the reverse shocks of supernova remnants. As before (Silvia et al. 2010), we use an idealized setup of a planar shock impacting a dense, spherical clump implanted with a population of Lagrangian particles that act as tracers of dust. These tracers represent a distribution of dust grains that vary in both species and size. Specifically, we investigate those cases in which the cloud initially has super-solar metal abundances (Z 1000 Z&sun;), as we expect the ejecta knots from supernova explosions to be extremely metal-enriched. A high abundance of metals has significant influence on both the cooling properties of the cloud and the thermal sputtering rates of the embedded dust grains. We also include a brief discussion about the difficulty of using the piecewise parabolic method for solving the hydrodynamic equations with high cooling rates produced by high metallicities. Through these simulations, we seek to quantify the fragmentation of ejecta clumps for comparison to observations of nearby supernova remnants and calculate the dust survival rate for these heavily metal-enriched cases. Estimates for dust survival in supernova shocks is critical in determining the source of dust at high redshift.

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