The evolution of protoplanetary disc radii and disc masses in star-forming regions

Marchington, Bridget; Parker, R. J.

doi:10.1093/mnras/stac2145

Cited by 3 publications

(1 citation statement)

References 112 publications

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“…The high-UV environment is expected to heat and photoevaporate protoplanetary disks around young stars in the cluster, driving mass loss via a wind and truncating the disks' radii (Johnstone et al 1998;Störzer & Hollenbach 1999;Adams et al 2004;Clarke 2007;Winter et al 2018;Sellek et al 2020;Marchington & Parker 2022;. This impacts the physical and chemical properties of the disks (Walsh et al 2013;Boyden & Eisner 2023) and the planet formation process occurring within (Throop & Bally 2005;Haworth et al 2018;Qiao et al 2023).…”

Section: Introductionmentioning

confidence: 99%

Isolating Dust and Free–Free Emission in ONC Proplyds with ALMA Band 3 Observations

Ballering,

Cleeves,

Haworth

et al. 2023

ApJ

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The Orion Nebula Cluster (ONC) hosts protoplanetary disks experiencing external photoevaporation by the cluster’s intense UV field. These “proplyds” are comprised of a disk surrounded by an ionization front. We present ALMA Band 3 (3.1 mm) continuum observations of 12 proplyds. Thermal emission from the dust disks and free–free emission from the ionization fronts are both detected, and the high-resolution (0.″057) of the observations allows us to spatially isolate these two components. The morphology is unique compared to images at shorter (sub)millimeter wavelengths, which only detect the disks, and images at longer centimeter wavelengths, which only detect the ionization fronts. The disks are small (r d = 6.4–38 au), likely due to truncation by ongoing photoevaporation. They have low spectral indices (α ≲ 2.1) measured between Bands 7 and 3, suggesting the dust emission is optically thick. They harbor tens of Earth masses of dust as computed from the millimeter flux using the standard method although their true masses may be larger due to the high optical depth. We derive their photoevaporative mass-loss rates in two ways: first, by invoking ionization equilibrium and second, by using the brightness of the free–free emission to compute the density of the outflow. We find decent agreement between these measurements and M ̇ = 0.6–18.4 × 10−7 M ⊙ yr−1. The photoevaporation timescales are generally shorter than the ∼1 Myr age of the ONC, underscoring the known “proplyd lifetime problem.” Disk masses that are underestimated due to being optically thick remains one explanation to ease this discrepancy.

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Section: Introductionmentioning

confidence: 99%

Isolating Dust and Free–Free Emission in ONC Proplyds with ALMA Band 3 Observations

Ballering,

Cleeves,

Haworth

et al. 2023

ApJ

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The Sun’s Birth Environment: Context for Meteoritics

Desch,

Miret-Roig

2024

Space Sci Rev

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Meteorites trace planet formation in the Sun’s protoplanetary disk, but they also record the influence of the Sun’s birth environment. Whether the Sun formed in a region like Taurus-Auriga with $\sim 10^{2}$ ∼ 10 2 stars, or a region like the Carina Nebula with $\sim 10^{6}$ ∼ 10 6 stars, matters for how large the Sun’s disk was, for how long and from how far away it accreted gas from the molecular cloud, and how it acquired radionuclides like 26Al. To provide context for the interpretation of meteoritic data, we review what is known about the Sun’s birth environment. Based on an inferred gas disk outer radius $\approx 50 - 90$ ≈ 50 − 90 AU, radial transport in the disk, and the abundances of noble gases in Jupiter’s atmosphere, the Sun’s molecular cloud and protoplanetary disk were exposed to an ultraviolet flux $G_{0} \sim 30 - 3000$ G 0 ∼ 30 − 3000 during its birth and first $\approx 10$ ≈ 10 Myr of evolution. Based on the orbits of Kuiper Belt objects, the Solar System was subsequently exposed to a stellar density $\approx \, 100 \, M_{\odot } \, {\mathrm{pc}}^{-3}$ ≈ 100 M ⊙ pc − 3 for $\approx 100$ ≈ 100 Myr, strongly implying formation in a bound cluster. These facts suggest formation in a region like the outskirts of the Orion Nebula, perhaps 2 pc from the center. The protoplanetary disk might have accreted gas for many Myr, but a few $\times 10^{5}$ × 10 5 yr seems more likely. It probably inherited radionuclides from its molecular cloud, enriched by inputs from supernovae and especially Wolf-Rayet star winds, and acquired a typical amount of 26Al.

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fried v2: a new grid of mass-loss rates for externally irradiated protoplanetary discs

Haworth,

Coleman,

Qiao

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We present a new fried grid of mass loss rates for externally far-ultraviolet (FUV) irradiated protoplanetary discs. As a precursor to the new grid, we also explore the microphysics of external photoevaporation, determining the impact of polycyclic aromatic hydrocarbon (PAH) abundance, metallicity, coolant depletion (via freeze out and radial drift) and grain growth (depletion of small dust in the outer disc) on disc mass loss rates. We find that metallicity variations typically have a small effect on the mass loss rate, since the impact of changes in heating, cooling and optical depth to the disc approximately cancel out. The new fried grid therefore focuses on i) expanding the basic physical parameter space (disc mass, radius, UV field, stellar mass) ii) on enabling variation of the the PAH abundance and iii) including an option for grain growth to have occurred or not in the disc. What we suggest is the fiducial model is comparable to the original fried grid. When the PAH-to-dust ratio is lower, or the dust in the wind more abundant, the mass loss rate can be substantially lower. We demonstrate with a small set of illustrative disc evolutionary calculations that this in turn can have a significant impact on the disc mass/radius/ evolution and lifetime.

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The evolution of protoplanetary disc radii and disc masses in star-forming regions

Cited by 3 publications

References 112 publications

Isolating Dust and Free–Free Emission in ONC Proplyds with ALMA Band 3 Observations

Isolating Dust and Free–Free Emission in ONC Proplyds with ALMA Band 3 Observations

The Sun’s Birth Environment: Context for Meteoritics

fried v2: a new grid of mass-loss rates for externally irradiated protoplanetary discs

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