A tree algorithm reduces multi-component coagulation complexity from O(N^{2d}) to O(d N^d log N) by grouping similar interactions and matches direct-method results in tests with analytic solutions.
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Common analytic approximations underestimate protoplanetary disk millimeter continuum emission by 10-15%, causing overestimates of optical depth, mass, and temperature in SED analyses.
Irregular hexahedral dust grains yield nearly the same polarization morphology and fraction as spherical grains in self-scattering regimes but with up to 2.5 times higher scattering opacity, and are still insufficient to match observed polarization levels.
Numerical simulations of porous fractal and consolidated particles show stronger forward scattering, broader polarization peaks, and lower absorption per unit mass than compact spheres, implying larger dust masses from observed fluxes.
citing papers explorer
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A fast tree algorithm for multi-component coagulation equation
A tree algorithm reduces multi-component coagulation complexity from O(N^{2d}) to O(d N^d log N) by grouping similar interactions and matches direct-method results in tests with analytic solutions.
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Millimeter dust continuum and polarization in protoplanetary disks with scattering: A slab model
Common analytic approximations underestimate protoplanetary disk millimeter continuum emission by 10-15%, causing overestimates of optical depth, mass, and temperature in SED analyses.
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Exploring Polarized Millimeter Emission from Protoplanetary Disks with Irregular Dust Grains
Irregular hexahedral dust grains yield nearly the same polarization morphology and fraction as spherical grains in self-scattering regimes but with up to 2.5 times higher scattering opacity, and are still insufficient to match observed polarization levels.
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Modeling (Sub-)millimeter Scattering Properties of Fractal and Consolidated Porous Particles: Applications to Protoplanetary Disks
Numerical simulations of porous fractal and consolidated particles show stronger forward scattering, broader polarization peaks, and lower absorption per unit mass than compact spheres, implying larger dust masses from observed fluxes.