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

Long, Feng; Andrews, Sean M.; Rosotti, Giovanni; Harsono, Daniel; Pinilla, P.; Wilner, David J.; Öberg, Karin I.; Teague, Richard; Trapman, Leon; Tabone, B.

doi:10.3847/1538-4357/ac634e

Cited by 41 publications

(30 citation statements)

References 89 publications

(135 reference statements)

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“…Table 5 shows the CO gas disk size measurements, and both R CO (gray) and R edge (red) are marked in Figure 14. Overall, we find R CO values that are generally consistent with those reported in Long et al (2022). We do, however, find considerably smaller R CO values for the V4046 Sgr (20%) and DoAr 25 (30%) disks.…”

Section: A Few Emission Surfaces Present Substructures In the Formsupporting

confidence: 89%

“…We do, however, find considerably smaller R CO values for the V4046 Sgr (20%) and DoAr 25 (30%) disks. For the V4046 Sgr disk, this is likely driven by the coarse angular resolution (1″) of the CO observations used by Long et al (2022), while for the DoAr 25 disk, the ability to draw a wedge precisely along the CO emission surface to avoid confusion from the disk midplane likely leads to an improved estimate of R CO .…”

Section: A Few Emission Surfaces Present Substructures In the Formmentioning

confidence: 99%

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CO Line Emission Surfaces and Vertical Structure in Midinclination Protoplanetary Disks

Law

Crystian

Teague

et al. 2022

ApJ

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High spatial resolution CO observations of midinclination (≈30°–75°) protoplanetary disks offer an opportunity to study the vertical distribution of CO emission and temperature. The asymmetry of line emission relative to the disk major axis allows for a direct mapping of the emission height above the midplane, and for optically thick, spatially resolved emission in LTE, the intensity is a measure of the local gas temperature. Our analysis of Atacama Large Millimeter/submillimeter Array archival data yields CO emission surfaces, dynamically constrained stellar host masses, and disk atmosphere gas temperatures for the disks around the following: HD 142666, MY Lup, V4046 Sgr, HD 100546, GW Lup, WaOph 6, DoAr 25, Sz 91, CI Tau, and DM Tau. These sources span a wide range in stellar masses (0.50–2.10 M ⊙), ages (∼0.3–23 Myr), and CO gas radial emission extents (≈200–1000 au). This sample nearly triples the number of disks with mapped emission surfaces and confirms the wide diversity in line emitting heights (z/r ≈ 0.1 to ≳0.5) hinted at in previous studies. We compute the radial and vertical CO gas temperature distributions for each disk. A few disks show local temperature dips or enhancements, some of which correspond to dust substructures or the proposed locations of embedded planets. Several emission surfaces also show vertical substructures, which all align with rings and gaps in the millimeter dust. Combining our sample with literature sources, we find that CO line emitting heights weakly decline with stellar mass and gas temperature, which, despite large scatter, is consistent with simple scaling relations. We also observe a correlation between CO emission height and disk size, which is due to the flared structure of disks. Overall, CO emission surfaces trace ≈2–5× gas pressure scale heights (Hg) and could potentially be calibrated as empirical tracers of Hg.

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Section: A Few Emission Surfaces Present Substructures In the Formsupporting

confidence: 89%

Section: A Few Emission Surfaces Present Substructures In the Formmentioning

confidence: 99%

CO Line Emission Surfaces and Vertical Structure in Midinclination Protoplanetary Disks

Law

Crystian

Teague

et al. 2022

ApJ

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“…Observations indicate that the gas and dust radii may be similar (e.g. Ansdell et al 2018), although gas radii are likely to be higher by a factor of around two (Sanchis et al 2021;Long et al 2022) and simulations show the dust radius moves with the gas radius during disc evolution (both inward evolution due to external photoevaporation, and outward evolution due to viscous spreading, (Sellek et al 2020)).…”

Section: Discussionmentioning

confidence: 99%

“…However, we note that although the dust radius may follow the gas radius during photoevaporation, the two are by no means the same. Sanchis et al (2021) and Long et al (2022) find that the gas radii of discs in nearby star-forming regions (Lupus, ρ Oph and Upper Sco) are at least a factor of two larger than the dust radii.…”

Section: Disc Photoevaporation and Evolutionmentioning

confidence: 99%

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

Marchington

Parker

2022

Monthly Notices of the Royal Astronomical Society

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Protoplanetary discs are crucial to understanding how planets form and evolve, but these objects are subject to the vagaries of the birth environments of their host stars. In particular, photoionising radiation from massive stars has been shown to be an effective agent in disrupting protoplanetary discs. External photoevaporation leads to the inward evolution of the radii of discs, whereas the internal viscous evolution of the disc causes the radii to evolve outwards. We couple N-body simulations of star-forming regions with a post-processing analysis of disc evolution to determine how the radius and mass distributions of protoplanetary discs evolve in young star-forming regions. To be consistent with observations, we find that the initial disc radii must be of order 100 au, even though these discs are readily destroyed by photoevaporation from massive stars. Furthermore, the observed disc radii distribution in the Orion Nebula Cluster is more consistent with moderate initial stellar densities (100 M⊙ pc−3), in tension with dynamical models that posit much higher inital densities for the ONC. Furthermore, we cannot reproduce the observed disc radius distribution in the Lupus star-forming region if its discs are subject to external photoevaporation. A more detailed comparison is not possible due to the well-documented uncertainties in determining the ages of pre-main sequence (disc-hosting) stars.

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“…Young planets forming in such disks have now been directly observed in the PDS70 system (Keppler et al 2018;Müller et al 2018;Haffert et al 2019). Recent disk surveys show that these disks have an inherent scatter in their global quantities, such as masses and radii (Ansdell et al 2016;Pascucci et al 2016;Tazzari et al 2017;Ansdell et al 2018;Andrews 2020;van der Marel & Mulders 2021;Long et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Combined effects of disc winds and turbulence-driven accretion on planet populations

Alessi

2022

Monthly Notices of the Royal Astronomical Society

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Recent surveys show that protoplanetary disks have lower levels of turbulence than expected based on their observed accretion rates. A viable solution to this is that magnetized disk winds dominate angular momentum transport. This has several important implications for planet formation processes. We compute the physical and chemical evolution of disks and the formation and migration of planets under the combined effects of angular momentum transport by turbulent viscosity and disk winds. We take into account the critical role of planet traps to limit Type I migration in all of these models and compute thousands of planet evolution tracks for single planets drawn from a distribution of initial disk properties and turbulence strengths. We do not consider multi-planet models nor include N-body planet-planet interactions. Within this physical framework we find that populations with a constant value disk turbulence and winds strength produce mass-semimajor axis distributions in the M-a diagram with insufficient scatter to compare reasonably with observations. However, populations produced as a consequence of sampling disks with a distribution of the relative strengths of disk turbulence and winds fit much better. Such models give rise to a substantial super Earth population at orbital radii 0.03-2 AU, as well as a clear separation between the produced hot Jupiter and warm Jupiter populations. Additionally, this model results in a good comparison with the exoplanetary mass-radius distribution in the M-R diagram after post-disk atmospheric photoevaporation is accounted for.

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

Cited by 41 publications

References 89 publications

CO Line Emission Surfaces and Vertical Structure in Midinclination Protoplanetary Disks

CO Line Emission Surfaces and Vertical Structure in Midinclination Protoplanetary Disks

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

Combined effects of disc winds and turbulence-driven accretion on planet populations

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