Contacts of Water Ice in Protoplanetary Disks—Laboratory Experiments

Musiolik, Grzegorz; Wurm, Gerhard

doi:10.3847/1538-4357/ab0428

Cited by 138 publications

(134 citation statements)

References 43 publications

(49 reference statements)

Supporting

Mentioning

127

Contrasting

Order By: Relevance

“…The fragmentation velocity V frag has been experimentally studied for silicates, water ice and CO 2 ice (Blum & Wurm 2008;Wada et al 2009;Güttler et al 2010;Yamamoto et al 2014;Musiolik et al 2016;Musiolik & Wurm 2019) and has been shown to be dependent on the dust composition. Fragmentation velocities are in the range between 1 m s −1 (silicates) and several tens of m s −1 (icy aggregates, see Gonzalez et al 2015 for a detailed review).…”

Section: Snow Lines As Discontinuities In Fragmentation Thresholdmentioning

confidence: 99%

Self-induced dust traps around snow lines in protoplanetary discs

Vericel

Gonzalez

2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

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.

show abstract

Section: Snow Lines As Discontinuities In Fragmentation Thresholdmentioning

confidence: 99%

Self-induced dust traps around snow lines in protoplanetary discs

Vericel

Gonzalez

2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Silicate grains have a fragmentation threshold ∼ 1 m s −1 while icy dust fragments for a relative velocity larger than several 10 m s −1 (Blum & Wurm 2008;Yamamoto et al 2014). While recent laboratory experiments (Gundlach et al 2018;Musiolik & Wurm 2019) found lower surface energies for water ice than previously used at low temperatures, thus suggesting that ice is not more resistant than silicates, they disagree with the tensile strengths measured in numerical simulations by Tatsuuma et al (2019). Further investigation is thus needed before the issue can be settled.…”

Section: Growth Modelmentioning

confidence: 94%

Evolution of porous dust grains in protoplanetary discs – I. Growing grains

Garcia

Gonzalez

2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

One of the main problems in planet formation, hampering the growth of small dust to planetesimals, is the so-called radial-drift barrier. Pebbles of cm to dm sizes are thought to drift radially across protoplanetary discs faster than they can grow to larger sizes, and thus to be lost to the star. To overcome this barrier, drift has to be slowed down or stopped, or growth needs to be sped up. In this paper, we investigate the role of porosity on both drift and growth.We have developed a model for porosity evolution during grain growth and applied it to numerical simulations of protoplanetary discs. We find that growth is faster for porous grains, enabling them to transition to the Stokes drag regime, decouple from the gas, and survive the radial-drift barrier. Direct formation of small planetesimals from porous dust is possible over large areas of the disc.

show abstract

“…This mechanism relies on a high sticking behavior of dust grains, which are typically assumed to be icy at locations relevant to our work. Recently, Musiolik & Wurm (2019) investigated this property in the laboratory for mm-sized water ice grains and found that their stickiness at very low temperatures is similar to that of silicates, thus unfavorable for fluffy grain growth. But whether this collisional behavior is also prevalent for sub-mm particles is still an open question.…”

Section: Discussionmentioning

confidence: 99%

Predicting the Observational Signature of Migrating Neptune-sized Planets in Low-viscosity Disks

Weber¹,

Pérez

Benítez-Llambay³

et al. 2019

ApJ

View full text Add to dashboard Cite

The migration of planetary cores embedded in a protoplanetary disk is an important mechanism within planetformation theory, relevant for the architecture of planetary systems. Consequently, planet migration is actively discussed, yet often results of independent theoretical or numerical studies are unconstrained due to the lack of observational diagnostics designed in light of planet migration. In this work we follow the idea of inferring the migration behavior of embedded planets by means of the characteristic radial structures that they imprint in the disk's dust density distribution. We run hydrodynamical multifluid simulations of gas and several dust species in a locally isothermal α-disk in the low-viscosity regime (α = 10 −5 ) and investigate the obtained dust structures. In this framework, a planet of roughly Neptune mass can create three (or more) rings in which dust accumulates. We find that the relative spacing of these rings depends on the planet's migration speed and direction. By performing subsequent radiative transfer calculations and image synthesis we show that -always under the condition of a near-inviscid disk -different migration scenarios are, in principle, distinguishable by long-baseline, state-of-the-art ALMA observations.

show abstract

Contacts of Water Ice in Protoplanetary Disks—Laboratory Experiments

Cited by 138 publications

References 43 publications

Self-induced dust traps around snow lines in protoplanetary discs

Self-induced dust traps around snow lines in protoplanetary discs

Evolution of porous dust grains in protoplanetary discs – I. Growing grains

Predicting the Observational Signature of Migrating Neptune-sized Planets in Low-viscosity Disks

Contact Info

Product

Resources

About