Probing protoplanetary disk evolution in the Chamaeleon II region

Villenave, M.; Ménard, F.; Dent, W. R. F.; Benisty, M.; Plas, G. van der; Williams, Jonathan P.; Ansdell, Megan; Ribas, Álvaro; Cáceres, C.; Cánovas, H.; Cieza, Lucas A.; Hales, Antonio; Kamp, I.; Pinte, C.; Principe, David A.; Schreiber, M. R.

doi:10.1051/0004-6361/202140496

Cited by 16 publications

(19 citation statements)

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“…Millimeter interferometry is one of the best ways to measure the bulk properties of disks, in particular their masses, sizes, and large-scale spatial features (e.g., Williams and Cieza 2011). ALMA's combination of sensitivity and resolution has enabled near-complete surveys of these bulk properties for disk populations across all the major nearby star-forming regions (e.g., Ansdell et al 2016;Barenfeld et al 2016;Pascucci et al 2016;Eisner et al 2018;Ruíz-Rodríguez et al 2018;Cazzoletti et al 2019;Grant et al 2021;Villenave et al 2021;van Terwisga et al 2022), which have led to a significant improvement of detection rate and number of surveyed regions (see Fig. 1).…”

Section: Protoplanetary Disk Masses and Sizes From MM Interferometrymentioning

confidence: 99%

“…By sampling star-forming regions with different ages, the recent ALMA surveys have been able to demonstrate that, in general, the continuum emission, interpreted as disk dust mass, systematically decreases with the age of the region (e.g., Ansdell et al 2016Ansdell et al , 2017Barenfeld et al 2016;Pascucci et al 2016;Eisner et al 2018;Ruíz-Rodríguez et al 2018;Cox et al 2017;van Terwisga et al 2019van Terwisga et al , 2020Villenave et al 2021, see Fig. 5), likely reflecting disk dispersal, dust evolution and/or grain growth (e.g., Pinilla et al 2020).…”

Section: Disk Dust Mass As a Function Of Agementioning

confidence: 99%

“…Alcalá et al (2014Alcalá et al ( , 2017, for Chamaeleon I fromManara et al (2016Manara et al ( , 2017b, for Upper Scorpius fromManara et al (2020). For the remaining regions, we collected data fromTesti et al (2022) for Ophiuchus and Corona Australis, fromVillenave et al (2021) for Chamaeleon II, and from Herczeg and Hillenbrand (2014) when possible, for Taurus, with some information from other works (e.g.,Ingleby et al 2013;Manara et al 2014;Alcalá et al 2021; …”

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confidence: 99%

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Demographics of young stars and their protoplanetary disks: lessons learned on disk evolution and its connection to planet formation

Manara¹,

Ansdell²,

Rosotti³

et al. 2022

Preprint

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Since Protostars and Planets VI (PPVI), our knowledge of the global properties of protoplanetary and debris disks, as well as of young stars, has dramatically improved. At the time of PPVI, mm-observations and optical to near-infrared spectroscopic surveys were largely limited to the Taurus star-forming region, especially of its most massive disk and stellar population. Now, near-complete surveys of multiple star-forming regions cover both spectroscopy of young stars and mm interferometry of their protoplanetary disks. This provides an unprecedented statistical sample of stellar masses and mass accretion rates, as well as disk masses and radii, for almost 1000 young stellar objects within 300 pc from us, while also sampling different evolutionary stages, ages, and environments. At the same time, surveys of debris disks are revealing the bulk properties of this class of more evolved objects. This chapter reviews the statistics of these measured global star and disk properties and discusses their constraints on theoretical models describing global disk evolution. Our comparisons of observations to theoretical model predictions extends beyond the traditional viscous evolution framework to include analytical descriptions of magnetic wind effects. Finally, we discuss how recent observational results can provide a framework for models of planet population synthesis and planet formation.

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Section: Protoplanetary Disk Masses and Sizes From MM Interferometrymentioning

confidence: 99%

Section: Disk Dust Mass As a Function Of Agementioning

confidence: 99%

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confidence: 99%

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Demographics of young stars and their protoplanetary disks: lessons learned on disk evolution and its connection to planet formation

Manara¹,

Ansdell²,

Rosotti³

et al. 2022

Preprint

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“…Furthermore, the disk mass content is crucial to determine whether planet formation may occur. Disk population studies in nearby star-forming regions (e.g., Barenfeld et al 2016;Ansdell et al 2016;Testi et al 2016;Pascucci et al 2016;Cieza et al 2019;Williams et al 2019;Sanchis et al 2020;Villenave et al 2021) proved that the scaling relation between disk mass and stellar mass is steeper than linear. Therefore, it appears that disks in the low-stellar-mass regime do not possess enough material to form the known planetary systems (Manara et al 2018), unless the planet-formation efficiency is 100% (Mulders et al 2021).…”

Section: Implications For Planet Formation Around Vlm Starsmentioning

confidence: 99%

A giant planet shaping the disk around the very low mass star CIDA 1

Curone,

Izquierdo,

Testi

et al. 2022

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Context. Exoplanetary research has provided us with exciting discoveries of planets around very low mass (VLM) stars (0.08 M M 0.3 M ; e.g., TRAPPIST-1 and Proxima Centauri). However, current theoretical models still strive to explain planet formation in these conditions and do not predict the development of giant planets. Recent high-resolution observations from the Atacama Large Millimeter/submillimeter Array (ALMA) of the disk around CIDA 1, a VLM star in Taurus, show substructures hinting at the presence of a massive planet. Aims. We aim to reproduce the dust ring of CIDA 1, observed in the dust continuum emission in ALMA Band 7 (0.9 mm) and Band 4 (2.1 mm), along with its 12 CO (J = 3 − 2) and 13 CO (J = 3 − 2) channel maps, assuming the structures are shaped by the interaction of the disk with a massive planet. We seek to retrieve the mass and position of the putative planet, through a global simulation assessing planet-disk interaction to quantitatively reproduce protoplanetary disk observations of both dust and gas emission in a self-consistent way. Methods. We model the protoplanetary disk with a set of hydrodynamical simulations, hosting an embedded planet with a starting mass between 0.1 and 4.0 M Jup initially located at a distance between 9 and 11 au from the central star. We compute the dust and gas emission using radiative transfer simulations, and, finally, we obtain the synthetic observations treating the images as the actual ALMA observations. Results. Our models indicate that a planet with a minimum mass of ∼ 1.4 M Jup orbiting at a distance of ∼ 9 − 10 au can explain the morphology and location of the observed dust ring at Band 7 and Band 4. We match the flux of the dust emission observation with a dust-to-gas mass ratio in the disk of ∼ 10 −2 . We are able to reproduce the low spectral index (∼ 2) observed where the dust ring is detected, with a ∼ 40 − 50% fraction of optically thick emission. Assuming a 12 CO abundance of 5 × 10 −5 and a 13 CO abundance 70 times lower, our synthetic images reproduce the morphology of the 12 CO (J = 3 − 2) and 13 CO (J = 3 − 2) observed channel maps where the cloud absorption allowed a detection. From our simulations, we estimate that a stellar mass M = 0.2 M and a systemic velocity sys = 6.25 km s −1 are needed to reproduce the gas rotation as retrieved from molecular line observations. Applying an empirical relation between planet mass and gap width in the dust, we predict a maximum planet mass of ∼ 4 − 8 M Jup . Conclusions. Our results suggest the presence of a massive planet orbiting CIDA 1, thus challenging our understanding of planet formation around VLM stars.

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“…While there are numerous observations of protoplanetary disks (e.g., Andrews 2020), and various aspects of their evolution have been modeled theoretically, the properties of such protoplanetary disks are still not well constrained. Indeed, we still do not have a complete picture of the evolution of even our own protosolar nebula (e.g., Villenave et al 2021).…”

Section: Introductionmentioning

confidence: 99%

The Effect of Accretion Rate and Composition on the Structure of Ice-rich Super-Earths

Lozovsky

Prialnik

Podolak

2022

ApJ

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It is reasonable to assume that the structure of a planet and the interior distribution of its components are determined by its formation history. We thus follow the growth of a planet from a small embryo through its subsequent evolution. We estimate the accretion rate range based on a protoplanetary disk model at a large-enough distance from the central star for water ice to be a major component. We assume the accreted material to be a mixture of silicate rock and ice, with no H–He envelope, as the accretion timescale is much longer than the time required for the nebular gas to dissipate. We adopt a thermal evolution model that includes accretional heating, radioactive energy release, and separation of ice and rock. Taking the Safronov parameter and the ice-to-rock ratio as free parameters, we compute growth and evolutionary sequences for different parameter combinations, for 4.6 Gyr. We find the final structure to depend significantly on both parameters. Low initial ice-to-rock ratios and high accretion rates, each resulting in an increased heating rate, lead to the formation of extended rocky cores, while the opposite conditions leave the composition almost unchanged and result in relatively low internal temperatures. When rocky cores form, the ice-rich outer mantles still contain rock mixed with the ice. We find that a considerable fraction of the ice evaporates upon accretion, depending on parameters, and assume it is lost, thus the final surface composition and bulk density of the planet do not necessarily reflect the protoplanetary disk composition.

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Probing protoplanetary disk evolution in the Chamaeleon II region

Cited by 16 publications

References 59 publications

Demographics of young stars and their protoplanetary disks: lessons learned on disk evolution and its connection to planet formation

Demographics of young stars and their protoplanetary disks: lessons learned on disk evolution and its connection to planet formation

A giant planet shaping the disk around the very low mass star CIDA 1

The Effect of Accretion Rate and Composition on the Structure of Ice-rich Super-Earths

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