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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Simulations demonstrate that gas-dust interactions produce radial offsets between micron and millimeter dust in gas-bearing debris disks, depending on gas mass, optical depth, and small-grain abundance.
citing papers explorer
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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.
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The ALMA survey to Resolve exoKuiper belt Substructures (ARKS) XI: Gas-dust interactions and radial offsets between micron and millimetre-sized grains
Simulations demonstrate that gas-dust interactions produce radial offsets between micron and millimeter dust in gas-bearing debris disks, depending on gas mass, optical depth, and small-grain abundance.