The paradox of youth for ALMA planet candidates

Nayakshin, Sergei

doi:10.1093/mnras/staa246

Cited by 6 publications

(3 citation statements)

References 132 publications

(182 reference statements)

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“…One of the first images to come from ALMA was the now famous HL Tau disc, a disc surrounding a young, nearby star in the Taurus star-forming region [67]. Further observational studies, in particular, the Disc Substructures at High Angular Resolution Project (DSHARP) [68], have shown that discs around young stars display features than can be attributed to a change in disc composition [69][70][71][72] as a function of radius, or the presence of fledgling planets within those discs [73][74][75][76][77] (although the latter scenario is still hotly debated [78,79]).…”

Section: Destruction Of Protoplanetary Discsmentioning

confidence: 99%

The birth environment of planetary systems

Parker

2020

R. Soc. open sci.

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Star and planet formation are inextricably linked. In the earliest phases of the collapse of a protostar, a disc forms around the young star and such discs are observed for the first several million years of a star’s life. It is within these circumstellar, or protoplanetary, discs that the first stages of planet formation occur. Recent observations from the Atacama large millimetre array (ALMA) suggest that planet formation may already be underway after only 1 Myr of a star’s life. However, stars do not form in isolation; they form from the collapse and fragmentation of giant molecular clouds several parsecs in size. This results in young stars forming in groups—often referred to as ‘clusters’. In these star-forming regions, the stellar density is much higher than the location of the Sun and other stars in the Galactic disc that host exoplanets. As such, the environment where stars form has the potential to influence the planet formation process. In star-forming regions, protoplanetary discs can be truncated or destroyed by interactions with passing stars, as well as photoevaporation from the radiation fields of very massive stars. Once formed, the planets themselves can have their orbits altered by dynamical encounters—either directly from passing stars or through secondary effects such as the Kozai–Lidov mechanism. In this contribution, I review the different processes that can affect planet formation and stability in star-forming regions. I discuss each process in light of the typical range of stellar densities observed for star-forming regions. I finish by discussing these effects in the context of theories for the birth environment of the Solar System.

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Section: Destruction Of Protoplanetary Discsmentioning

confidence: 99%

The birth environment of planetary systems

Parker

2020

R. Soc. open sci.

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“…One of the first images to come from ALMA was the now famous HL Tau disc, a disc surrounding a young, nearby star in the Taurus star-forming region [63]. Further observational studies, in particular the Disk Substructures at High Angular Resolution Project (DSHARP) [64], have shown that discs around young stars display features than can be attributed to a change in disc composition [65][66][67][68] as a function of radius, or the presence of fledgling planets within those discs [69][70][71][72][73] (although the latter scenario is still hotly debated [74,75]).…”

Section: Destruction Of Protoplanetary Discsmentioning

confidence: 99%

The birth environment of planetary systems

Parker¹

2020

Preprint

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Star and planet formation are inextricably linked. In the earliest phases of the collapse of a protostar a disc forms around the young star and such discs are observed for the first several million years of a star's life. It is within these circumstellar, or protoplanetary, discs that the first stages of planet formation occur. Recent observations from ALMA suggest that planet formation may already be well under way after only 1 Myr of a star's life. However, stars do not form in isolation; they form from the collapse and fragmentation of giant molecular clouds several parsecs in size. This results in young stars forming in groups -often referred to as 'clusters'. In these star-forming regions the stellar density is much higher than the location of the Sun, and other stars in the Galactic disc that host exoplanets. As such, the environment where stars form has the potential to influence the planet formation process. In star-forming regions, protoplanetary discs can be truncated or destroyed by interactions with passing stars, as well as photoevaporation from the radiation fields of very massive stars. Once formed, the planets themselves can have their orbits altered by dynamical encounters -either directly from passing stars or through secondary effects such as the Kozai-Lidov mechanism. In this contribution, I review the different processes that can affect planet formation and stability in star-forming regions. I discuss each process in light of the typical range of stellar densities observed for star-forming regions. I finish by discussing these effects in the context of theories for the birth environment of the Solar System.

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“…On the other hand, high-resolution imaging toward a targeted group of disks has shown that large and massive disks are often associated with substructures, mostly seen as gaps and rings (e.g., Partnership et al 2015;Andrews et al 2018a;Long et al 2018;Cieza et al 2021), but also as arcs and spiral arms (van der Marel et al 2013;Huang et al 2018b;Dong et al 2018). Given the ubiquitous nature of planetary systems in the Galaxy (e.g., Winn & Fabrycky 2015), the frequent appearance of disk substructures suggests that they might be relevant to the process of planet formation, though establishing the direct connection between a disk feature and a planet is so far challenging, considering the complex physics involved in disk and planet evolution (e.g., Nayakshin 2020).…”

Section: Introductionmentioning

confidence: 99%

A Large Double-ring Disk Around the Taurus M Dwarf J04124068+2438157

Long

Ren

Wallack

et al. 2023

ApJ

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Planet formation imprints signatures on the physical structures of disks. In this paper, we present high-resolution (∼50 mas, 8 au) Atacama Large Millimeter/submillimeter Array observations of 1.3 mm dust continuum and CO line emission toward the disk around the M3.5 star 2MASS J04124068+2438157. The dust disk consists of only two narrow rings at radial distances of 0.″47 and 0.″78 (∼70 and 116 au), with Gaussian σ widths of 5.6 and 8.5 au, respectively. The width of the outer ring is smaller than the estimated pressure scale height by ∼25%, suggesting dust trapping in a radial pressure bump. The dust disk size, set by the location of the outermost ring, is significantly larger (by 3σ) than other disks with similar millimeter luminosity, which can be explained by an early formation of local pressure bump to stop radial drift of millimeter dust grains. After considering the disk’s physical structure and accretion properties, we prefer planet–disk interaction over dead zone or photoevaporation models to explain the observed dust disk morphology. We carry out high-contrast imaging at the L ′ band using Keck/NIRC2 to search for potential young planets, but do not identify any source above 5σ. Within the dust gap between the two rings, we reach a contrast level of ∼7 mag, constraining the possible planet below ∼2–4 M Jup. Analyses of the gap/ring properties suggest that an approximately Saturn-mass planet at ∼90 au is likely responsible for the formation of the outer ring, which can potentially be revealed with JWST.

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The paradox of youth for ALMA planet candidates

Cited by 6 publications

References 132 publications

The birth environment of planetary systems

The birth environment of planetary systems

The birth environment of planetary systems

A Large Double-ring Disk Around the Taurus M Dwarf J04124068+2438157

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