JWST observations at 15 and 25.5 μm reveal a smooth, radially broad debris disk around γ Ophiuchi extending to 250 au, interpreted as a steady-state collisional cascade from a wide planetesimal belt with possible low-eccentricity planetary perturbation.
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11 Pith papers cite this work. Polarity classification is still indexing.
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JWST observations of Sz 65 and Sz 66 reveal higher cold-to-hot water ratios in the secondary disk, attributed to its unstructured dust disk enabling efficient pebble drift across the snow line.
Non-ideal MHD shearing-box simulations with a new damping scheme yield power-law scalings for wind-driven accretion rates based on midplane plasma beta, ambipolar Elsasser number, and active layer thickness that match results within a factor of 2-3.
Spectral decomposition of 26 T Tauri disks finds Mg-rich silicate dust with 5-24% crystallinity and correlations linking annealed silica to stronger CO2 emission and forsterite to stronger H2O emission.
ALMA survey detects H2CO in 45% of 20 disks and finds strong correlations of line luminosity with disk size, mass, and stellar luminosity, suggesting grain-surface formation.
Accretion increases observable water mass in disks by expanding the emitting area via higher central luminosity, while viscous heating has no effect.
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.
Numerical experiments demonstrate that one migrating planet produces multiple long-lived dust rings and gaps in radiative discs through migration jumps, with cooling affecting jump count but not structure lifetime.
Multi-technique observations constrain the configuration of the ξ Tau system, detecting orbital oscillations on multiple timescales and suggesting component C is itself a binary.
Stronger radiation environments produce more massive, hotter protostellar discs whose fragments are large and disruptive rather than planetary-mass.
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Beyond the $\alpha$ model: scaling the wind-driven accretion rate in protoplanetary disks using systematic non-ideal magnetohydrodynamical simulations
Non-ideal MHD shearing-box simulations with a new damping scheme yield power-law scalings for wind-driven accretion rates based on midplane plasma beta, ambipolar Elsasser number, and active layer thickness that match results within a factor of 2-3.