Numerical simulations of Neptune's migration yield empirical expressions for eccentricity thresholds and capture efficiencies into exterior mean motion resonances, depending on migration rate, distance, and resonance order.
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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.
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Numerical estimation of the capture ability of Neptunian mean motion resonances
Numerical simulations of Neptune's migration yield empirical expressions for eccentricity thresholds and capture efficiencies into exterior mean motion resonances, depending on migration rate, distance, and resonance order.
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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.