Papers › The external photoevaporation of structured protoplanetary disks
The external photoevaporation of structured protoplanetary disks
Matías Gárate, Paola Pinilla, Thomas J. Haworth, Stefano Facchini
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The dust in planet-forming disks evolve rapidly through growth and radial drift, and external photoevaporation also contributes to this evolution in massive star-forming regions. We test whether the presence of substructures can explain the survival of the dust component and observed millimeter continuum emission in protoplanetary disks located within massive star-forming regions. We also characterize the dust content removed by the photoevaporative winds. For this, we performed hydrodynamical simulations of protoplanetary disks subject to irradiation fields of F_(UV) = 10², 10³, and 10⁴ G₀, with different dust trap locations. We used the FRIED grid to derive the mass loss rate for each irradiation field and disk properties, and then measure the evolution of the dust mass over time. For each simulation we estimate continuum emission at λ= 1.3 mm along with the radii encompassing 90% of the continuum flux, and characterize the dust size distribution entrained in the photoevaporative winds, along with the resulting far-ultraviolet (FUV) cross section. Our simulations show that the presence of dust traps can extend the lifetime of the dust component of the disk to a few millionyears if the FUV irradiation is F_(UV) ≲10³ G₀, but only if the dust traps are located inside the photoevaporative truncation radius. The dust component of a disk quickly disperse if the FUV irradiation is strong (10⁴ G₀) or if the substructures are located outside the photoevaporation radius. We do find however, that the dust grains entrained with the photoevaporative winds may result in an absorption FUV cross section of σ≈10⁻²² cm² at early times of evolution ($<$0.1 Myr), which is enough to trigger a self-shielding effect that reduces the total mass loss rate, and slow down the disk dispersal in a negative feedback loop process.
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