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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15 Pith papers cite this work. Polarity classification is still indexing.
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Semi-analytical model links observed scattering-surface height to small-dust mass, yielding global mass fractions of order 10^{-3} consistent with modest grain growth in ten protoplanetary disks.
Porous elongated dust grains exhibit decreasing intrinsic polarization with rising porosity and 90-degree polarization flips at specific wavelength-to-size ratios, enabling a new multi-wavelength method to constrain grain porosity in protoplanetary disks.
N-body simulations find stellar mass-loss effects dominate gravitational scattering in altering giant planet orbits around white dwarfs formed in star clusters, independent of density and initial conditions.
Low-column-density filaments align parallel to magnetic fields while high-column-density wide filaments align perpendicular, with transition at roughly 0.8-8 x 10^21 cm^-2; projection effects analyzed statistically.
Semi-analytical theory derives radial scalings for forced disk eccentricity (E ~ r^{-1} or r^{-2}) and resonance criteria for precessing binaries, plus a conjecture that cavity size tunes the ground eccentric mode to the binary precession frequency.
Observational study of MBM12 shows CO-to-H2 conversion factor near galactic average with density-dependent variations, high virial parameters decreasing at small scales, broken power-law mass-size relations indicating external pressure, and magnetic field orientation transition at N(H2) = 4.5e21 cm-
ALMA observations of 100 Ophiuchus discs show substructures linked to giant planet formation are common in discs above 10 Earth masses of dust and increase from Class I to Class II stages.
Halos in Elias 2-24, IM Lup, and DM Tau hold 20-30% of total dust mass with cm-sized grains, helping resolve the disk mass-budget problem even though drift and growth timescales are shorter than disk ages.
3D modeling of L1506C with THEMIS 2 dust model shows evolved grains needed in densest regions, indicating early grain growth in prestellar phase.
H-type objects in IC348 show spatial distributions matching stars and brown dwarfs, unlike the more dispersed distribution of simulated ejected planets, indicating a star-like formation origin.
Giant planet formation traps dust in pressure bumps and planetesimal formation converts dust to larger bodies, making evolved disk masses appear low as a natural outcome of these processes, with models matching observations best for initial disk masses of 4-7% solar mass.
A millimeter survey detects disks around five Herbig Be stars and shows no evidence of rapid disk dissipation with increasing stellar mass.
SKAO will enable the first large-scale high-resolution surveys of cm-wavelength disk emission to constrain dust growth, pebble demographics, and planet formation processes.
The paper reviews techniques for measuring protostellar accretion, analyzes methodological differences and caveats in comparing observations with simulations, and outlines next steps for a fuller picture.
citing papers explorer
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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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Interpreting the scattering surface in protoplanetary disks
Semi-analytical model links observed scattering-surface height to small-dust mass, yielding global mass fractions of order 10^{-3} consistent with modest grain growth in ten protoplanetary disks.
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Intrinsic polarisation of elongated porous dust grains
Porous elongated dust grains exhibit decreasing intrinsic polarization with rising porosity and 90-degree polarization flips at specific wavelength-to-size ratios, enabling a new multi-wavelength method to constrain grain porosity in protoplanetary disks.
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White dwarf planets in star clusters: gravitational scattering versus mass-loss effects
N-body simulations find stellar mass-loss effects dominate gravitational scattering in altering giant planet orbits around white dwarfs formed in star clusters, independent of density and initial conditions.
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Statistical analysis of the relative orientations between filaments and magnetic fields using Herschel and Planck data in star-forming regions
Low-column-density filaments align parallel to magnetic fields while high-column-density wide filaments align perpendicular, with transition at roughly 0.8-8 x 10^21 cm^-2; projection effects analyzed statistically.
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Insights from Analytical Theory of Eccentric Circumbinary Disks II. Forced Modes and Resonance for Precessing Binaries
Semi-analytical theory derives radial scalings for forced disk eccentricity (E ~ r^{-1} or r^{-2}) and resonance criteria for precessing binaries, plus a conjecture that cavity size tunes the ground eccentric mode to the binary precession frequency.
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B-Fields and Star Formation across Scales with TRAO (B-FROST): CO Abundances, Dynamics and Relative Orientations in the Translucent High Latitude Cloud MBM12
Observational study of MBM12 shows CO-to-H2 conversion factor near galactic average with density-dependent variations, high virial parameters decreasing at small scales, broken power-law mass-size relations indicating external pressure, and magnetic field orientation transition at N(H2) = 4.5e21 cm-
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The Ophiuchus DIsc Survey Employing ALMA (ODISEA). Substructures as a function of SED Class and disc mass in 100 systems
ALMA observations of 100 Ophiuchus discs show substructures linked to giant planet formation are common in discs above 10 Earth masses of dust and increase from Class I to Class II stages.
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Dust characterization of halos: The extended emission in protoplanetary disks
Halos in Elias 2-24, IM Lup, and DM Tau hold 20-30% of total dust mass with cm-sized grains, helping resolve the disk mass-budget problem even though drift and growth timescales are shorter than disk ages.
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Tracing grain growth in the forming prestellar core L1506C with 3D modeling of Herschel, IRAM, and CFHT observations
3D modeling of L1506C with THEMIS 2 dust model shows evolved grains needed in densest regions, indicating early grain growth in prestellar phase.
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Planet or brown dwarf? Constraints on the formation of H-type objects in IC348
H-type objects in IC348 show spatial distributions matching stars and brown dwarfs, unlike the more dispersed distribution of simulated ejected planets, indicating a star-like formation origin.
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A giant solution to the disk mass budget problem of planet formation
Giant planet formation traps dust in pressure bumps and planetesimal formation converts dust to larger bodies, making evolved disk masses appear low as a natural outcome of these processes, with models matching observations best for initial disk masses of 4-7% solar mass.
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A $\lambda=1.3$ millimeter Survey for Disks around Herbig Be Stars
A millimeter survey detects disks around five Herbig Be stars and shows no evidence of rapid disk dissipation with increasing stellar mass.
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Demographics of planet-forming disks with the SKAO
SKAO will enable the first large-scale high-resolution surveys of cm-wavelength disk emission to constrain dust growth, pebble demographics, and planet formation processes.
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The Accretion Process on Protostars
The paper reviews techniques for measuring protostellar accretion, analyzes methodological differences and caveats in comparing observations with simulations, and outlines next steps for a fuller picture.