The impact of planet wakes on the location and shape of the water ice line in a protoplanetary disk

Ziampras, Alexandros; Ataiee, Sareh; Kley, W.; Dullemond, C. P.

doi:10.1051/0004-6361/201936495

Cited by 34 publications

(31 citation statements)

References 37 publications

(44 reference statements)

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“…Similar to Ziampras et al (2020), the planet's presence is described by an additional gravitational force. We accounted for the shift of the system barycenter that is caused by the planet, but neglected backreaction of the disk onto the star and planet.…”

Section: Numericsmentioning

confidence: 99%

Importance of radiative effects in gap opening by planets in protoplanetary disks

Ziampras

Kley

Dullemond

2020

A&A

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Recent ALMA observations revealed concentric annular structures in several young class-II objects. In an attempt to produce the rings and gaps in some of these systems, they have been modeled numerically with a single embedded planet assuming a locally isothermal equation of state. This is often justified by observations targeting the irradiation-dominated outer regions of disks (approximately 100 au). We test this assumption by conducting hydrodynamics simulations of embedded planets in thin locally isothermal and radiative disks that mimic the systems HD 163296 and AS 209 in order to examine the effect of including the energy equation in a seemingly locally isothermal environment as far as planet-disk interaction is concerned. We find that modeling such disks with an ideal equation of state makes a difference in terms of the number of produced rings and the spiral arm contrast in the disk. Locally isothermal disks produce sharper annular or azimuthal features and overestimate a single planet's gap-opening capabilities by producing multiple gaps. In contrast, planets in radiative disks carve a single gap for typical disk parameters. Consequently, for accurate modeling of planets with semimajor axes up to about 100 au, radiative effects should be taken into account even in seemingly locally isothermal disks. In addition, for the case of AS 209, we find that the primary gap is significantly different between locally isothermal and radiative models. Our results suggest that multiple planets are required to explain the ring-rich structures in such systems.

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Section: Numericsmentioning

confidence: 99%

Importance of radiative effects in gap opening by planets in protoplanetary disks

Ziampras

Kley

Dullemond

2020

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“…& Wurm 2019;Ros et al 2019;Vericel & Gonzalez 2020;Ziampras et al 2020). In future studies, we plan to improve our model by introducing H 2 O, CO, and CO 2 snow lines and adopting dust fragmentation velocity (u frag ) depending on the position of dust particle relative to the snow line.…”

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confidence: 99%

Gravitoviscous protoplanetary disks with a dust component

Elbakyan

Johansen²,

Lambrechts³

et al. 2020

A&A

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Aims. We study the dynamics and growth of dust particles in circumstellar disks of different masses that are prone to gravitational instability during the critical first Myr of their evolution. Methods. We solved the hydrodynamics equations for a self-gravitating and viscous circumstellar disk in a thin-disk limit using the FEOSAD numerical hydrodynamics code. The dust component is made up of two different components: micron-sized dust and grown dust of evolving size. For the dust component, we considered the dust coagulation, fragmentation, momentum exchange with the gas, and dust self-gravity. Results. We found that the micron-sized dust particles grow rapidly in the circumstellar disk, reaching a few cm in size in the inner 100 au of the disk during less than 100 kyr after the disk formation, provided that fragmentation velocity is 30 ms−1. Due to the accretion of micron dust particles from the surrounding envelope, which serves as a micron dust reservoir, the approximately cm-sized dust particles continue to be present in the disk for more than 900 kyr after the disk formation and maintain a dust-to-gas ratio close to 0.01. We show that a strong correlation exists between the gas and pebble fluxes in the disk. We find that radial surface density distribution of pebbles in the disk shows power-law distribution with an index similar to that of the Minimum-mass solar nebula regardless the disk mass. We also show that the gas surface density in our models agrees well with measurements of dust in protoplanetary disks of AS 209, HD 163296, and DoAr 25 systems. Conclusions. Pebbles are formed during the very early stages of protoplanetary disk evolution. They play a crucial role in the planet formation process. Our disc simulations reveal the early onset (<105 yr) of an inwards-drifting flux of pebble-sized particles that makes up approximately between one hundredth and one tenth of the gas mass flux, which appears consistent with mm-observations of discs. Such a pebble flux would allow for the formation of planetesimals by streaming instability and the early growth of embryos by pebble accretion. We conclude that unlike the more common studies of isolated steady-state protoplanetary disks, more sophisticated global numerical simulations of circumstellar disk formation and evolution, including the pebble formation from the micron dust particles, are needed for performing realistic planet formation studies.

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“…We have assumed that the presence of a planet with a low mass undergoing type-I migration does not disturb the disc's overall structure enough to destroy the pressure and migration trap at the ice line. However, this might not be true for massive planets, which may even be able to change the temperature of the disc and reshape the water-ice line (Ziampras et al 2020). The influence of a massive planet on the pressure and migration trap at the ice line in discs that feature a transition in the dust fragmentation velocity is beyond the scope of the present work and will be investigated in a future study.…”

Section: Migration Trapmentioning

confidence: 90%

The water-ice line as a birthplace of planets: implications of a species-dependent dust fragmentation threshold

Müller

Savvidou

Bitsch

2021

A&A

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The thermodynamic structure of protoplanetary discs is determined by dust opacities, which depend on the size of the dust grains and their chemical composition. In the inner regions, the grain sizes are regulated by the level of turbulence (e.g. α viscosity) and by the dust fragmentation velocity that represents the maximal velocity that grains can have at a collision before they fragment. Here, we perform self-consistently calculated 2D hydrodynamical simulations that consider a full grain size distribution of dust grains with a transition in the dust fragmentation velocity at the water-ice line. This approach accounts for the results of previous particle collision laboratory experiments, in which silicate particles typically have a lower dust fragmentation velocity than water-ice particles. Furthermore, we probe the effects of variations in the water abundance, the dust-to-gas ratio, and the turbulence parameter on the disc structure. For the discs with a transition in the dust fragmentation velocity at the water-ice line, we find a narrow but striking zone of planetary outward migration, including for low viscosities. In addition, we find a bump in the radial pressure gradient profile that tends to be located slightly inside the ice line. Both of these features are present for all tested disc parameters. Thus, we conclude that the ice line can function both as a migration trap, which can extend the growth times of planets before they migrate to the inner edge of the protoplanetary disc, and as a pressure trap, where planetesimal formation can be initiated or enhanced.

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The impact of planet wakes on the location and shape of the water ice line in a protoplanetary disk

Cited by 34 publications

References 37 publications

Importance of radiative effects in gap opening by planets in protoplanetary disks

Importance of radiative effects in gap opening by planets in protoplanetary disks

Gravitoviscous protoplanetary disks with a dust component

The water-ice line as a birthplace of planets: implications of a species-dependent dust fragmentation threshold

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