On the secular evolution of the ratio between gas and dust radii in protoplanetary discs

Toci, Claudia; Rosotti, Giovanni; Lodato, Giuseppe; Testi, L.; Trapman, Leon

doi:10.1093/mnras/stab2112

Cited by 42 publications

(42 citation statements)

References 106 publications

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“…Lodato et al (2017) explained this scatter by assuming long viscous timescales and a dispersion in disc ages but under-predict it in the older region of Upper Scorpius (Manara et al 2020). Sellek et al (2020) invoked fast dust radial drift to increase the scatter but this scenario is in tension with disc sizes measured from dust emission (Toci et al 2021).…”

Section: Introductionmentioning

confidence: 99%

MHD disc winds can reproduce fast disc dispersal and the correlation between accretion rate and disc mass in Lupus

Tabone

Rosotti

Lodato

et al. 2021

Monthly Notices of the Royal Astronomical Society: Letters

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The final architecture of planetary systems depends on the extraction of angular momentum and mass-loss processes of the discs in which they form. Theoretical studies proposed that magnetized winds launched from the discs (MHD disc winds) could govern accretion and disc dispersal. In this work, we revisit the observed disc demographics in the framework of MHD disc winds, combining analytical solutions of disc evolution and a disc population synthesis approach. We show that MHD disc winds alone can account for both disc dispersal and accretion properties. The decline of disc fraction over time is reproduced by assuming that the initial accretion timescale (a generalization of the viscous timescale) varies from disc to disc and that the decline of the magnetic field strength is slower than that of the gas. The correlation between accretion rate and disc mass, and the dispersion of the data around the mean trend as observed in Lupus is then naturally reproduced. The model also accounts for the rapidity of the disc dispersal. This paves the way for planet formation models in the paradigm of wind-driven accretion.

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Section: Introductionmentioning

confidence: 99%

MHD disc winds can reproduce fast disc dispersal and the correlation between accretion rate and disc mass in Lupus

Tabone

Rosotti

Lodato

et al. 2021

Monthly Notices of the Royal Astronomical Society: Letters

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“…Among Class II disks such a large ratio between gas disk size and dust disk size is a sign of substantial dust evolution, which seems unlikely for these young sources (see, e.g. Trapman et al 2019;Rosotti et al 2019;Toci et al 2021). It thus seems difficult to reconcile the picture of wind-driven disk evolution with observed disk sizes at all disk ages.…”

Section: Comparing To Observationsmentioning

confidence: 99%

Effect of MHD wind-driven disk evolution on the observed sizes of protoplanetary disks

Trapman,

Tabone,

Rosotti

et al. 2021

Preprint

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It is still unclear whether the evolution of protoplanetary disks, a key ingredient in the theory of planet formation, is driven by viscous turbulence or magnetic disk winds. As viscously evolving disks expand outward over time, the evolution of disk sizes is a discriminant test for studying disk evolution. However, it is unclear how the observed disk size changes over time if disk evolution is driven by magnetic disk winds. Combining the thermochemical code DALI with the analytical wind-driven disk evolution model presented in Tabone et al.(2021a), we study the time evolution of the observed gas outer radius as measured from CO rotational emission (R CO, 90% ). The evolution of R CO, 90% is driven by the evolution of the disk mass, as the physical radius stays constant over time. For a constant α DW , an extension of the α−Shakura-Sunyaev parameter to wind-driven accretion, R CO, 90% decreases linearly with time. Its initial size is set by the disk mass and the characteristic radius R c,0 , but only R c,0 affects the evolution of R CO, 90% , with a larger R c,0 resulting in a steeper decrease of R CO, 90% . For a time-dependent α DW , R CO, 90% stays approximately constant during most of the disk lifetime until R CO, 90% rapidly shrinks as the disk dissipates. The constant α DW -models are able to reproduce the observed gas disk sizes in the ∼ 1 − 3 Lupus and ∼ 5 − 11 Myr old Upper Sco star-forming regions. However, they likely overpredict the gas disk size of younger ( 0.7 Myr) disks.

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“…Such a large gas disk will affect the dust evolution in GO Tau. As a point of comparison, we selected a model from the Toci et al (2021) grids that has a similar R CO to the GO Tau disk. We also re-ran the simulation with a perturbed version of this model, with two pressure bumps added to mimic the morphology of the mm continuum emission rings at 73 and 110 au, respectively.…”

Section: The Most Extended Co Disk Of Go Taumentioning

confidence: 99%

Gas Disk Sizes from CO Line Observations: A Test of Angular Momentum Evolution

Long,

Andrews,

Rosotti

et al. 2022

Preprint

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The size of a disk encodes important information about its evolution. Combining new Submillimeter Array (SMA) observations with archival Atacama Large Millimeter Array (ALMA) data, we analyze mm continuum and CO emission line sizes for a sample of 44 protoplanetary disks around stars with masses of 0.15-2 M in several nearby star-forming regions. Sizes measured from 12 CO line emission span from 50 to 1000 au. This range could be explained by viscous evolution models with different α values (mostly of 10 −4 − 10 −3 ) and/or a spread of initial conditions. The CO sizes for most disks are also consistent with MHD wind models that directly remove disk angular momentum, but very large initial disk sizes would be required to account for the very extended CO disks in the sample. As no CO size evolution is observed across stellar ages of 0.5-20 Myr in this sample, determining the dominant mechanism of disk evolution will require a more complete sample for both younger and more evolved systems. We find that the CO emission is universally more extended than the continuum emission by an average factor of 2.9 ± 1.2. The ratio of the CO to continuum sizes does not show any trend with stellar mass, mm continuum luminosity, or the properties of substructures. The GO Tau disk has the most extended CO emission in this sample, with an extreme CO to continuum size ratio of 7.6. Seven additional disks in the sample show high size ratios ( 4) that we interpret as clear signs of substantial radial drift.

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On the secular evolution of the ratio between gas and dust radii in protoplanetary discs

Cited by 42 publications

References 106 publications

MHD disc winds can reproduce fast disc dispersal and the correlation between accretion rate and disc mass in Lupus

MHD disc winds can reproduce fast disc dispersal and the correlation between accretion rate and disc mass in Lupus

Effect of MHD wind-driven disk evolution on the observed sizes of protoplanetary disks

Gas Disk Sizes from CO Line Observations: A Test of Angular Momentum Evolution

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