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.
Monthly Notices of the Royal Astronomical Society518(3), 4481–4493 (2023)
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The disk instability model remains viable for explaining giant planets that form early, at large orbital distances, and around M-dwarf stars, supported by updated simulations and observations.
citing papers explorer
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Dust characterization of halos: The extended emission in protoplanetary disks
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.
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Giant Planet Formation by Disk Instability
The disk instability model remains viable for explaining giant planets that form early, at large orbital distances, and around M-dwarf stars, supported by updated simulations and observations.