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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3 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
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astro-ph.EP 3years
2026 3verdicts
UNVERDICTED 3representative citing papers
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.
Forward modeling of synthetic debris disc images demonstrates that recovered scattering phase functions are biased by observational limits and do not directly reflect intrinsic dust properties.
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.
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What you see is not necessarily what you get: Interpreting near-infrared scattering phase functions of debris discs
Forward modeling of synthetic debris disc images demonstrates that recovered scattering phase functions are biased by observational limits and do not directly reflect intrinsic dust properties.