The external photoevaporation of planet-forming discs

Winter, Andrew J.; Haworth, Thomas J.

doi:10.1140/epjp/s13360-022-03314-1

Cited by 46 publications

(19 citation statements)

References 354 publications

(510 reference statements)

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“…This leaves an additional mechanism for mass removal by external photoevaporation (e.g. Matsuyama et al 2003;Winter & Haworth 2022). This is supported by observational findings that discs near massive stars have lower masses than others (Ansdell et al 2017;van Terwisga et al 2020) and that clusters with a low ambient radiation field have longer disc lifetimes (Michel et al 2021).…”

Section: Introductionmentioning

confidence: 66%

Towards a population synthesis of discs and planets. II. Confronting disc models and observations at the population level

Emsenhuber¹,

Burn²,

Weder³

et al. 2023

Preprint

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Aims. We want to find the distribution of initial conditions that best reproduces disc observations at the population level. Methods. We first ran a parameter study using a 1D model that includes the viscous evolution of a gas disc, dust, and pebbles, coupled with an emission model to compute the millimetre flux observable with ALMA. This was used to train a machine learning surrogate model that can compute the relevant quantity for comparison with observations in seconds. This surrogate model was used to perform parameter studies and synthetic disc populations.Results. Performing a parameter study, we find that internal photoevaporation leads to a lower dependency of disc lifetime on stellar mass than external photoevaporation. This dependence should be investigated in the future. Performing population synthesis, we find that under the combined losses of internal and external photoevaporation, discs are too short lived. Conclusions. To match observational constraints, future models of disc evolution need to include one or a combination of the following processes: infall of material to replenish the discs, shielding of the disc from internal photoevaporation due to magnetically driven disc winds, and extinction of external high-energy radiation. Nevertheless, disc properties in low-external-photoevaporation regions can be reproduced by having more massive and compact discs. Here, the optimum values of the α viscosity parameter lie between 3 × 10 −4 and 10 −3 and with internal photoevaporation being the main mode of disc dispersal.

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Section: Introductionmentioning

confidence: 66%

Towards a population synthesis of discs and planets. II. Confronting disc models and observations at the population level

Emsenhuber¹,

Burn²,

Weder³

et al. 2023

Preprint

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“…While the environments studied here are much less extreme than e.g. the ONC, A0 and B-type stars for the are much more common, and similar radiation fields are encountered by a large fraction of young stars even in the Solar neighborhood (Winter & Haworth 2022). This emphasizes the need for planet population syntheses to take this process into account, as well as resolved studies of the disks in these radiation environments, in order to link the observed exoplanet population to the well-studied nearby protoplanetary disks.…”

Section: Discussionmentioning

confidence: 93%

“…As such, these regions do not represent the more massive, clustered environments in which most stars form (Lada & Lada 2003;Bressert et al 2010). The median star in the galaxy is formed in a region with a higher surface density of young stars, and -as a result of the stellar mass distribution -will be within a few pc of an O-or B-type young star at some point in its early life (Winter & Haworth 2022). These young, massive stars affect the survival of disks in nearby stars through photo-evaporation, as shown by the presence of proplyds (O'Dell et al 1993) and by theoretical work (e.g., Scally & Clarke 2001;Haworth et al 2018;Concha-Ramírez et al 2019;Emsenhuber et al 2023).…”

Section: Introductionmentioning

confidence: 99%

Survey of Orion Disks with ALMA (SODA)

Terwisga

Hacar

Dishoeck

et al. 2022

A&A

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Context. Surveys of protoplanetary disks in nearby star-forming regions (SFRs) have provided important information on their demographics. However, due to their sample sizes, these surveys cannot be used to study how disk properties vary with the environment. Aims. We conduct a survey of the unresolved millimeter continuum emission of 873 protoplanetary disks identified by Spitzer in the L1641 and L1647 regions of the Orion A cloud. This is the largest such survey yet, allowing us to identify even weak trends in the median disk mass as a function of position in the cloud and cluster membership. The sample detection rates and median masses are also compared to those of nearby (<300 pc) SFRs. Methods. The sample was observed with the Atacama Large Millimeter/submillimeter Array (ALMA) at 225 GHz, with a median rms of 0.08 mJy beam−1, or 1.5 M⊕. The data were reduced and imaged using an innovative parallel data processing approach. Results. We detected 58% (502/873) of the observed disks. This includes 20 disks with dust masses >100 M⊕, and two objects associated with extended dust emission. By fitting a log-normal distribution to the data, we infer a median disk dust mass in the full sample of 2.2−0.2+0.2 M⊕. In L1641 and L1647, median dust masses are 2.1−0.2+0.2M⊕ and 2.6−0.5+0.4M⊕, respectively. Conclusions. The disk mass distribution of the full sample is similar to that of nearby low-mass SFRs at similar ages of 1–3 Myr. We find only weak trends in disk (dust) masses with galactic longitude and between the Young Stellar Object (YSO) clusters identified in the sample, with median masses varying by ≲50%. Differences in age may explain the median disk mass variations in our subsamples. Apart from this, disk masses are essentially constant at scales of ~100 pc. This also suggests that the majority of disks, even in different SFRs, are formed with similar initial masses and evolve at similar rates, assuming no external irradiation, with disk mass loss rates of ~10−8 M⊙ yr−1.

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“…This results in terrestrial planets being able to survive in the former (although icy planets migrated to within 1 ) while they no longer exist in the latter. The link to the environment comes from the anticorrelation of disc lifetimes with external photoevaporation rate [ 163 ]. Absent this, disc lifetimes are correlated with their initial mass.…”

Section: Resultsmentioning

confidence: 99%

Planetary population synthesis and the emergence of four classes of planetary system architectures

2023

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Planetary population synthesis is a helpful tool to understand the physics of planetary system formation. It builds on a global model, meaning that the model has to include a multitude of physical processes. The outcome can be statistically compared with exoplanet observations. Here, we review the population synthesis method and then use one population computed using the Generation III Bern model to explore how different planetary system architectures emerge and which conditions lead to their formation. The emerging systems can be classified into four main architectures: Class I of near in situ compositionally ordered terrestrial and ice planets, Class II of migrated sub-Neptunes, Class III of mixed low-mass and giant planets, broadly similar to the Solar System, and Class IV of dynamically active giants without inner low-mass planets. These four classes exhibit distinct typical formation pathways and are characterised by certain mass scales. We find that Class I forms from the local accretion of planetesimals followed by a giant impact phase, and the final planet masses correspond to what is expected from such a scenario, the ‘Goldreich mass’. Class II, the migrated sub-Neptune systems form when planets reach the ‘equality mass’ where accretion and migration timescales are comparable before the dispersal of the gas disc, but not large enough to allow for rapid gas accretion. Giant planets form when the ‘equality mass’ allows for gas accretion to proceed while the planet is migrating, i.e. when the critical core mass is reached. The main discriminant of the four classes is the initial mass of solids in the disc, with contributions from the lifetime and mass of the gas disc. The distinction between mixed Class III systems and Class IV dynamically active giants is in part due to the stochastic nature of dynamical interactions, such as scatterings between giant planets, rather than the initial conditions only. The breakdown of system into classes allows to better interpret the outcome of a complex model and understand which physical processes are dominant. Comparison with observations reveals differences to the actual population, pointing at limitation of theoretical understanding. For example, the overrepresentation of synthetic super-Earths and sub-Neptunes in Class I systems causes these planets to be found at lower metallicities than in observations.

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The external photoevaporation of planet-forming discs

Cited by 46 publications

References 354 publications

Towards a population synthesis of discs and planets. II. Confronting disc models and observations at the population level

Towards a population synthesis of discs and planets. II. Confronting disc models and observations at the population level

Survey of Orion Disks with ALMA (SODA)

Planetary population synthesis and the emergence of four classes of planetary system architectures

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