Dust grain size distributions evolve from large-grain dominated at high redshift to MRN-like at low redshift, driven primarily by shattering and ISM accretion after stars supply initial large grains, reproducing z=0 dust masses and Milky Way extinction properties.
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Cosmological zoom-in simulations find that grain-grain shattering in diffuse ISM gas drives rising PAH mass fraction with time, naturally producing the observed PAH-metallicity relation and inverse qPAH-molecular gas trends.
MD simulations yield silicate grain shattering thresholds of ~6 km/s and post-collision size distributions inconsistent with power-law predictions from Jones et al. (1996) and Hirashita & Kobayashi (2013).
citing papers explorer
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Dust and Grain Size Evolution in Galaxy Simulations: What Matters and What Does Not
Dust grain size distributions evolve from large-grain dominated at high redshift to MRN-like at low redshift, driven primarily by shattering and ISM accretion after stars supply initial large grains, reproducing z=0 dust masses and Milky Way extinction properties.
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The Lifecycle and Emission Properties of PAHs in Cosmological Hydrodynamic Galaxy Formation Simulations
Cosmological zoom-in simulations find that grain-grain shattering in diffuse ISM gas drives rising PAH mass fraction with time, naturally producing the observed PAH-metallicity relation and inverse qPAH-molecular gas trends.
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Silicate cosmic dust grain collisions in the interstellar medium: A molecular dynamics study
MD simulations yield silicate grain shattering thresholds of ~6 km/s and post-collision size distributions inconsistent with power-law predictions from Jones et al. (1996) and Hirashita & Kobayashi (2013).