Coupled disc-chemistry and N-body simulations identify three classes of giant-planet atmospheres whose elemental ratios (N/O*, C/O*, C/N*, S/N*) trace gas-dominated, planetesimal-dominated, or drift-enhanced accretion in time-dependent discs.
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The β Pictoris debris disk is on average 1.5 times thicker vertically in the mid-infrared than at millimeter wavelengths, with a relatively constant scale height across radius and warping consistent with secular perturbations from inner giant planets.
citing papers explorer
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Planet formation in chemically diverse and evolving discs II. Chemical fingerprints in planetary atmospheres
Coupled disc-chemistry and N-body simulations identify three classes of giant-planet atmospheres whose elemental ratios (N/O*, C/O*, C/N*, S/N*) trace gas-dominated, planetesimal-dominated, or drift-enhanced accretion in time-dependent discs.
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The multi-wavelength vertical structure of the archetypal $\beta$ Pictoris debris disk
The β Pictoris debris disk is on average 1.5 times thicker vertically in the mid-infrared than at millimeter wavelengths, with a relatively constant scale height across radius and warping consistent with secular perturbations from inner giant planets.