Planetesimal formation starts at the snow line

Drążkowska, Joanna; Alibert, Yann

doi:10.1051/0004-6361/201731491

Cited by 275 publications

(295 citation statements)

References 69 publications

(122 reference statements)

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“…Article number, page 9 of 17 for for condensation compared to solar and sub-solar metallicity. This, however, needs to be tested with future models like of Drażkowska & Alibert (2017) that combine grain growth and drift with condensation and planetesimal formation. In addition the C/O ratio of giant planet host stars could help to distinguish if water ice condensation is the main driver of giant planet formation.…”

Section: Planet Formationmentioning

confidence: 99%

Influence of sub- and super-solar metallicities on the composition of solid planetary building blocks

Bitsch

Battistini

2019

A&A

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The composition of the protoplanetary disc is thought to be linked to the composition of the host star, where a higher overall metallicity of the host star provides more building blocks for planets. However, most of the planet formation simulations only link the stellar iron abundance [Fe/H] to planet formation and the iron abundance in itself is used as a proxy to scale all elements. On the other hand, large surveys of stellar abundances show that this is not true. We use here stellar abundances from the GALAH surveys to determine the average detailed abundances of Fe, Si, Mg, O, and C for a broad range of host star metallicities with [Fe/H] spanning from -0.4 to +0.4. Using an equilibrium chemical model that features the most important rock forming molecules as well as volatile contributions of H 2 O, CO 2 , CH 4 and CO, we calculate the chemical composition of solid planetary building blocks around stars with different metallicities. Solid building blocks that are formed entirely interior to the water ice line (T>150K) only show an increase in Mg 2 SiO 4 and a decrease in MgSiO 3 for increasing host star metallicity, related to the increase of Mg/Si for higher [Fe/H]. Solid planetary building blocks forming exterior to the water ice line (T<150K), on the other hand, show dramatic changes in their composition. In particular the water ice content decreases from around ∼50% at [Fe/H]=-0.4 to ∼6% at [Fe/H]=0.4 in our chemical model. This is mainly caused by the increasing C/O ratio with increasing [Fe/H], which binds most of the oxygen in gaseous CO and CO 2 , resulting in a small water ice fraction. Planet formation simulations coupled with the chemical model confirm these results by showing that the water ice content of super-Earths decreases with increasing host star metallicity due to the increased C/O ratio. This decrease of the water ice fraction has important consequences for planet formation, planetary composition and the eventual habitability of planetary systems formed around these high metallicity stars.

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Section: Planet Formationmentioning

confidence: 99%

Influence of sub- and super-solar metallicities on the composition of solid planetary building blocks

Bitsch

Battistini

2019

A&A

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“…It is worth noting that we did not take into account the diffusion of sublimated CO inwards and outwards of the snow line. However, it has been proven (for water) that the snow line can lead to a diffusion of material that could enhance the dust surface density just outside the snow line (Drążkowska & Alibert 2017). In their paper, they used a model similar to ours for the fragmentation thresholds and added the diffusion terms.…”

Section: Case Ii: V Fragin V Fragoutmentioning

confidence: 99%

“…When grains cross a snow line, one also expects a diffusion of freshly sublimated gas both inwards and outwards (Ciesla & Cuzzi 2006). Gas moving outwards and crossing the snow line condenses onto the surface of grains, increasing the dust surface density (Armitage et al 2016;Schoonenberg & Ormel 2017;Drążkowska & Alibert 2017, for the water snowline specifically). Both of these processes can help radially concentrate dust.…”

Section: Introductionmentioning

confidence: 99%

“…Water is also one of the most abundant volatile species in discs, leading to a substantial diffusion at the snow line location (Ida & Guillot 2016;Schoonenberg & Ormel 2017). The combination of these effects can trigger the streaming instability and form planetesimals in immediate proximity to the water snow line for weakly turbulent discs (Drążkowska & Alibert 2017). Observations show that the water snow line also potentially affects the occurence of giant planets (Fernandes et al 2019).…”

Section: Introductionmentioning

confidence: 99%

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Self-induced dust traps around snow lines in protoplanetary discs

Vericel

Gonzalez

2019

Monthly Notices of the Royal Astronomical Society

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Dust particles need to grow efficiently from micrometre sizes to thousands of kilometres to form planets. With the growth of millimetre to meter sizes being hindered by a number of barriers, the recent discovery that dust evolution is able to create "self-induced" dust traps shows promises. The condensation and sublimation of volatile species at certain locations, called snow lines, is also thought to be an important part of planet formation scenarios. Given that dust sticking properties change across a snow line, this raises the question: how do snow lines affect the self-induced dust trap formation mechanism? The question is particularly relevant with the multiple observations of the carbon monoxide (CO) snow line in protoplanetary discs, since its effect on dust growth and dynamics is yet to be understood. In this paper, we present the effects of snow lines in general on the formation of self-induced dust traps in a parameter study, then focus on the CO snow line. We find that for a range of parameters, a dust trap forms at the snow line where the dust accumulates and slowly grows, as found for the water snow line in previous work. We also find that, depending on the grains sticking properties on either side of the CO snow line, it could either be a starting or braking point for dust growth and drift. This could provide clues to understand the link between dust distributions and snow lines in protoplanetary disc observations.

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“…Dust growth is expected to be further facilitated around opacity transition regions (Drążkowska & Alibert 2017;Zhang et al 2015). Common dust opacity models are in principle densityand temperature-dependent-with boundaries defined at conditions where aggregates of certain composition change phasesuch that crossing between two opacity regimes can change the absorption/emission properties of the disk.…”

Section: Introductionmentioning

confidence: 99%

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

Ziampras

Ataiee

Kley

et al. 2020

A&A

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Context. Planets in accretion disks can excite spiral shocks, and-if massive enough-open gaps in their vicinity. Both of these effects can influence the overall disk thermal structure. Aims. We model planets of different masses and semimajor axes in disks of various viscosities and accretion rates to examine their impact on disk thermodynamics and highlight the mutable, non-axisymmetric nature of icelines in systems with massive planets. Methods. We conduct a parameter study using numerical hydrodynamics simulations where we treat viscous heating, thermal cooling and stellar irradiation as additional source terms in the energy equation, with some runs including radiative diffusion. Our parameter space consists of a grid containing different combinations of planet and disk parameters.Results. Both gap opening and shock heating can displace the iceline, with the effects being amplified for massive planets in optically thick disks. The gap region can split an initially hot (T > 170 K) disk into a hot inner disk and a hot ring just outside of the planet's location, while shock heating can reshape the originally axisymmetric iceline into water-poor islands along spirals. We also find that radiative diffusion does not alter the picture significantly in this context. Conclusions. Shock heating and gap opening by a planet can effectively heat up optically thick disks and in general move and/or reshape the water iceline. This can affect the gap structure and migration torques. It can also produce azimuthal features that follow the trajectory of spiral arms, creating hot zones, "islands" of vapor and ice around spirals which could affect the accretion or growth of icy aggregates.

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Planetesimal formation starts at the snow line

Cited by 275 publications

References 69 publications

Influence of sub- and super-solar metallicities on the composition of solid planetary building blocks

Influence of sub- and super-solar metallicities on the composition of solid planetary building blocks

Self-induced dust traps around snow lines in protoplanetary discs

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

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