Planetesimal Formation by Sublimation

Saito, Etsuko; Sirono, Sin-iti

doi:10.1088/0004-637x/728/1/20

Cited by 91 publications

(78 citation statements)

References 18 publications

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“…When the inward-drifting pebbles cross the snow line, they progressively sublimate until only small refractory (silicate dust) seeds remain (e.g., Saito & Sirono 2011;Morbidelli et al 2016). Observations of the interstellar medium and of interplanetary dust particles indicate that these dust seeds should be of submicron size, corresponding to τ s ∼ 10 −7 −10 −5 .…”

Section: Solid-to-gas Density Ratio Inside Of the Snow Linementioning

confidence: 99%

Formation of dust-rich planetesimals from sublimated pebbles inside of the snow line

Ida

Guillot

2016

A&A

108

104

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Context. For up to a few millions of years, pebbles must provide a quasi-steady inflow of solids from the outer parts of protoplanetary disks to their inner regions. Aims. We wish to understand how a significant fraction of the pebbles grows into planetesimals instead of being lost to the host star. Methods. We examined analytically how the inward flow of pebbles is affected by the snow line and under which conditions dust-rich (rocky) planetesimals form. When calculating the inward drift of solids that is due to gas drag, we included the back-reaction of the gas to the motion of the solids. Results. We show that in low-viscosity protoplanetary disks (with a monotonous surface density similar to that of the minimum-mass solar nebula), the flow of pebbles does not usually reach the required surface density to form planetesimals by streaming instability. We show, however, that if the pebble-to-gas-mass flux exceeds a critical value, no steady solution can be found for the solid-to-gas ratio. This is particularly important for low-viscosity disks (α < 10 −3 ) where we show that inside of the snow line, silicate-dust grains ejected from sublimating pebbles can accumulate, eventually leading to the formation of dust-rich planetesimals directly by gravitational instability.Conclusions. This formation of dust-rich planetesimals may occur for extended periods of time, while the snow line sweeps from several au to inside of 1 au. The rock-to-ice ratio may thus be globally significantly higher in planetesimals and planets than in the central star.

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Section: Solid-to-gas Density Ratio Inside Of the Snow Linementioning

confidence: 99%

Formation of dust-rich planetesimals from sublimated pebbles inside of the snow line

Ida

Guillot

2016

A&A

108

104

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“…Note that we did not consider the possibility that the dust surface density near the snowline increases because of sublimation or recondensation (e.g. Saito & Sirono 2011;Ros & Johansen 2013;Schoonenberg & Ormel 2017). …”

Section: Fiducial Calculationsmentioning

confidence: 99%

Satellitesimal Formation via Collisional Dust Growth in Steady Circumplanetary Disks

Shibaike

Okuzumi

Sasaki

et al. 2017

ApJ

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The icy satellites around Jupiter are considered to have formed in a circumplanetary disk. While previous models focused on the formation of satellites starting from satellitesimals, the question of how satellitesimals form from smaller dust particles has not been addressed so far. In this work, we study the possibility that satellitesimals form in situ in a circumplanetary disk. We calculate the radial distribution of the surface density and representative size of icy dust particles that grow by colliding with each other and drift toward the central planet in a steady circumplanetary disk with a continuous supply of gas and dust from the parent protoplanetary disk. The radial drift barrier is overcome if the ratio of the dust to gas accretion rates onto the circumplanetary disk,Ṁ d /Ṁ g , is high and the strength of turbulence, α, is not too low. The collision velocity is lower than the critical velocity of fragmentation when α is low. Taken together, we find that the conditions for satellitesimal formation via dust coagulation are given byṀ d /Ṁ g ≥ 1 and 10 −4 ≤ α < 10 −2 . The former condition is generally difficult to achieve, suggesting that the in-situ satellitesimal formation via particle sticking is viable only under an extreme condition. We also show that neither satellitesimal formation via the collisional growth of porous aggregates nor via streaming instability is viable as long asṀ d /Ṁ g is low.

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“…The current literature for explaining dust rings and gaps in protoplanetary disks is very rich and includes zonal flows from the magnetorotational instability (MRI; e.g., Johansen et al 2009;Uribe et al 2011;Dittrich et al 2013;Simon & Armitage 2014), spatial variations of the disk viscosity (e.g., Kretke & Lin 2007;Regály et al 2012;Flock et al 2015;Pinilla et al 2016), secular gravitational instability (e.g., Youdin 2011; Takahashi & Inutsuka 2014), instabilities originating from dust settling (Lorén-Aguilar & Bate 2015), self-sustained recycling of inner dust rings (Husmann et al 2016), particle growth by condensation near ice lines (Saito & Sirono 2011;Ros & Johansen 2013;Stammler et al 2017), sintering of dust particles that inhibits dust growth near the ice lines (Okuzumi et al 2016), and planet-disk interaction (e.g., Rice et al 2006;Zhu et al 2011;Gonzalez et al 2012;Pinilla et al 2012a;Dipierro et al 2016;Dong & Fung 2016;Rosotti et al 2016). Although the latter explanation is the most widely used to interpret current observations, it is not a unique possibility, and several of the listed processes can play an important role during the disk evolution.…”

Section: Introductionmentioning

confidence: 99%

Dust Density Distribution and Imaging Analysis of Different Ice Lines in Protoplanetary Disks

Pinilla

Pohl

Stammler

et al. 2017

ApJ

132

118

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Recent high angular resolution observations of protoplanetary disks at different wavelengths have revealed several kinds of structures, including multiple bright and dark rings. Embedded planets are the most used explanation for such structures, but there are alternative models capable of shaping the dust in rings as it has been observed. We assume a disk around a Herbig star and investigate the effect that ice lines have on the dust evolution, following the growth, fragmentation, and dynamics of multiple dust size particles, covering from 1 μm to 2 m sized objects. We use simplified prescriptions of the fragmentation velocity threshold, which is assumed to change radially at the location of one, two, or three ice lines. We assume changes at the radial location of main volatiles, specifically H 2 O, CO 2 , and NH 3 . Radiative transfer calculations are done using the resulting dust density distributions in order to compare with current multiwavelength observations. We find that the structures in the dust density profiles and radial intensities at different wavelengths strongly depend on the disk viscosity. A clear gap of emission can be formed between ice lines and be surrounded by ring-like structures, in particular between the H 2 O and CO 2 (or CO). The gaps are expected to be shallower and narrower at millimeter emission than at near-infrared, opposite to model predictions of particle trapping. In our models, the total gas surface density is not expected to show strong variations, in contrast to other gap-forming scenarios such as embedded giant planets or radial variations of the disk viscosity.

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Planetesimal Formation by Sublimation

Cited by 91 publications

References 18 publications

Formation of dust-rich planetesimals from sublimated pebbles inside of the snow line

Formation of dust-rich planetesimals from sublimated pebbles inside of the snow line

Satellitesimal Formation via Collisional Dust Growth in Steady Circumplanetary Disks

Dust Density Distribution and Imaging Analysis of Different Ice Lines in Protoplanetary Disks

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