A portable expression is derived to estimate water ice crystallinity from Fresnel peak strength in scattered-light spectra at ~90° angles, yielding 10-20% for the HD 181327 debris disk and ~50% for the d216-0939 protoplanetary disk.
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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.
Gas giants form sub-snowline in binaries via dust traps at the tidal truncation radius, with observed planet semi-major axes following a_planet = 0.569 r_t (R²=0.94).
Radiative-transfer simulations with common dust models generate a range of spectral indices but cannot reach the lowest observed emissivity indices in protostars without invoking unexpectedly large millimeter-sized grains.
citing papers explorer
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Constraints on the Crystallinity of Water Ice in Planet-forming Disks from Infrared Scattered-Light Spectra
A portable expression is derived to estimate water ice crystallinity from Fresnel peak strength in scattered-light spectra at ~90° angles, yielding 10-20% for the HD 181327 debris disk and ~50% for the d216-0939 protoplanetary disk.
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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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Sub-Snowline Formation of Gas-Giant Planets in Binary Systems
Gas giants form sub-snowline in binaries via dust traps at the tidal truncation radius, with observed planet semi-major axes following a_planet = 0.569 r_t (R²=0.94).
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Pristine composition or size evolution: Can current dust models reproduce emissivities observed in nearby protostars?
Radiative-transfer simulations with common dust models generate a range of spectral indices but cannot reach the lowest observed emissivity indices in protostars without invoking unexpectedly large millimeter-sized grains.