Measuring the ratio of the gas and dust emission radii of protoplanetary disks in the Lupus star-forming region

Sanchís, E.; Testi, L.; Natta, A.; Facchini, Stefano; Manara, C. F.; Miotello, A.; Ercolano, Barbara; Henning, Th.; Preibisch, Thomas; Carpenter, John M.; Gregorio-Monsalvo, I. de; Jayawardhana, Ray; López, C.; Mužić, Koraljka; Pascucci, Ilaria; Santamaría-Miranda, Alejandro; Terwisga, Sierk van; Williams, Jonathan P.

doi:10.1051/0004-6361/202039733

Cited by 59 publications

(75 citation statements)

References 96 publications

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“…However, it became clear thanks to the ALMA measurements that dust radii are smaller than gas radii by about a factor of 0.5 (Ansdell et al 2018), which we adopt to truncate the planetesimal disk. The recent study of Sanchis et al (2021) expand and confirm these results and further find no dependence of the CO to dust size ratio on the stellar mass.…”

Section: Disk Radiussupporting

confidence: 59%

The New Generation Planetary Population Synthesis (NGPPS)

Burn

Schlecker

Mordasini

et al. 2021

A&A

134

119

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Context. Previous theoretical works on planet formation around low-mass stars have often been limited to large planets and individual systems. As current surveys routinely detect planets down to terrestrial size in these systems, models have shifted toward a more holistic approach that reflects their diverse architectures. Aims. Here, we investigate planet formation around low-mass stars and identify differences in the statistical distribution of modeled planets. We compare the synthetic planet populations to observed exoplanets and we discuss the identified trends. Methods. We used the Generation III Bern global model of planet formation and evolution to calculate synthetic populations, while varying the central star from Solar-like stars to ultra-late M dwarfs. This model includes planetary migration, N-body interactions between embryos, accretion of planetesimals and gas, and the long-term contraction and loss of the gaseous atmospheres. Results. We find that temperate, Earth-sized planets are most frequent around early M dwarfs (0.3 M⊙–0.5 M⊙) and that they are more rare for Solar-type stars and late M dwarfs. The planetary mass distribution does not linearly scale with the disk mass. The reason behind this is attributed to the emergence of giant planets for M⋆ ≥ 0.5 M⊙, which leads to the ejection of smaller planets. Given a linear scaling of the disk mass with stellar mass, the formation of Earth-like planets is limited by the available amount of solids for ultra-late M dwarfs. For M⋆ ≥ 0.3 M⊙, however, there is sufficient mass in the majority of systems, leading to a similar amount of Exo-Earths going from M to G dwarfs. In contrast, the number of super-Earths and larger planets increases monotonically with stellar mass. We further identify a regime of disk parameters that reproduces observed M-dwarf systems such as TRAPPIST-1. However, giant planets around late M dwarfs, such as GJ 3512b, only form when type I migration is substantially reduced. Conclusions. We are able to quantify the stellar mass dependence of multi-planet systems using global simulations of planet formation and evolution. The results fare well in comparison to current observational data and predict trends that can be tested with future observations.

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Section: Disk Radiussupporting

confidence: 59%

The New Generation Planetary Population Synthesis (NGPPS)

Burn

Schlecker

Mordasini

et al. 2021

A&A

134

119

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“…However, the characteristic size of dust emission is mostly indicative of dust growth and drift processes rather than the true radial profile of the gas (Rosotti et al 2019a,b;Powell et al 2019). As such, the observation of a rather constant continuum size between Class 0, I and II discs of about 50 au (Tobin et al 2020;Sanchis et al 2021) should be interpreted with caution.…”

Section: Disc Sizementioning

confidence: 96%

“…Alternatively, characteristic emission radii of CO rotational lines have been measured, though on a smaller sample of sources due to sensitivity issues (Barenfeld et al 2017;Ansdell et al 2018;Sanchis et al 2021). However, this characteristic radius is indicative of the region of the disc where the CO lines become optically thin, either due to a drop in the surface density profile or a drop in CO abundance due to e.g., photodissociation (Trapman et al 2019).…”

Section: Disc Sizementioning

confidence: 99%

Secular evolution of MHD wind-driven discs: analytical solutions in the expanded α-framework

Tabone

Rosotti

Cridland

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The evolution of protoplanetary discs and the related process of planet formation is regulated by angular momentum transport and mass-loss processes. Over the past decade, the paradigm of viscosity has been challenged and MHD disc winds appear as a compelling scenario to account for disc accretion. In this work, we aim to construct the equivalent of the widely used analytical description of viscous evolution for the MHD wind case. The transport of angular momentum and mass induced by the wind is parameterized by an α-like parameter and by the magnetic lever arm parameter λ. Extensions of the paradigmatic Lynden-Bell and Pringle similarity solutions to the wind case are presented. We show that wind-driven accretion leads to a steeper decrease in the disc mass and accretion rate than in viscous models due to the absence of disc spreading. If the decline of the magnetic field strength is slower than that of the gas surface density, the disc is dispersed after a finite time. The evolution of the disc in the $\dot{M}_*-M_{D}$ plane is sensitive to the wind and turbulence parameters. A disc population evolving under the action of winds can exhibit a correlation between $\dot{M}_*$ and MD depending on the initial conditions. The simplified framework proposed in this work opens to a new avenue to test the effectiveness of wind-driven accretion from the observed disc demographics and constitutes an important step to include wind-driven accretion in planet population synthesis models.

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“…However, due of the low angular resolution of our data (elongated beam) and significant foreground absorption, we could not get a reliable estimate the gas sizes. Higher angular resolution observations and detailed modeling of each object is needed to estimate quantitatively the dust and gas sizes, and to compare the dust and gas size ratio with previous studies (e.g., Ansdell et al 2018;Facchini et al 2019;Trapman et al 2019;Sanchis et al 2021).…”

Section: Co Line Emissionmentioning

confidence: 99%

Probing protoplanetary disk evolution in the Chamaeleon II region

Villenave

Ménard

Dent

et al. 2021

A&A

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Context. Characterizing the evolution of protoplanetary disks is necessary to improve our understanding of planet formation. Constraints on both dust and gas are needed to determine the dominant disk dissipation mechanisms. Aims. We aim to compare the disk dust masses in the Chamaeleon II (Cha II) star-forming region with other regions with ages between 1 and 10 Myr. Methods. We use ALMA band 6 observations (1.3 mm) to survey 29 protoplanetary disks in Cha II. Dust mass estimates are derived from the continuum data. Results. Out of our initial sample of 29 disks, we detect 22 sources in the continuum, 10 in 12CO, 3 in 13CO, and none in C18O (J = 2−1). Additionally, we detect two companion candidates in the continuum and 12CO emission. Most disk dust masses are lower than 10 M⊕, assuming thermal emission from optically thin dust. Including non-detections, we derive a median dust mass of 4.5 ± 1.5 M⊕ from survival analysis. We compare consistent estimations of the distributions of the disk dust mass and the disk-to-stellar mass ratios in Cha II with six other low mass and isolated star-forming regions in the age range of 1–10 Myr: Upper Sco, CrA, IC 348, Cha I, Lupus, and Taurus. When comparing the dust-to-stellar mass ratio, we find that the masses of disks in Cha II are statistically different from those in Upper Sco and Taurus, and we confirm that disks in Upper Sco, the oldest region of the sample, are statistically less massive than in all other regions. Performing a second statistical test of the dust mass distributions from similar mass bins, we find no statistical differences between these regions and Cha II. Conclusions. We interpret these trends, most simply, as a sign of decline in the disk dust masses with time or dust evolution. Different global initial conditions in star-forming regions may also play a role, but their impact on the properties of a disk population is difficult to isolate in star-forming regions lacking nearby massive stars.

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Measuring the ratio of the gas and dust emission radii of protoplanetary disks in the Lupus star-forming region

Cited by 59 publications

References 96 publications

The New Generation Planetary Population Synthesis (NGPPS)

The New Generation Planetary Population Synthesis (NGPPS)

Secular evolution of MHD wind-driven discs: analytical solutions in the expanded α-framework

Probing protoplanetary disk evolution in the Chamaeleon II region

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