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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MD simulations of 5-50 Å silicate grains find shattering thresholds of ~6 km/s for both SiO2 and astrodust compositions, twice the canonical 2.7 km/s value, with shattered size distributions inconsistent with prior power-law predictions.
Dust attenuation follows a universal mass-dependent relation from z=0 to 7 with a transition at 10^9 solar masses where nebular attenuation steepens relative to stellar.
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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.