Collisions of CO${}_2$ Ice Grains in Planet Formation

Abstract

In protoplanetary disks, CO${}_2$ is solid ice beyond its snow line at $\sim 10\mathrm{AU}$. Due to its high abundance, it contributes heavily to the collisional evolution in this region of the disk. For the first time, we carried out laboratory collision experiments with CO${}_2$ ice particles and a CO${}_2$-covered wall at a temperature of 80 K. Collision velocities varied between 0 - 2.5 m/s. Particle sizes were on the order of $\sim$ 100 $\mu$m. We find a threshold velocity between the sticking and the bouncing regime at 0.04 m/s. Particles with greater velocities but below 1 m/s bounce off the wall. For yet greater velocities, fragmentation occurs. We give analytical models for the coefficients of restitution and fragmentation strength consistent with the experimental data. Set in context, our data show that CO${}_2$ ice and silicate dust resemble each other in the collisional behavior. Compared to water ice the sticking velocity is an order of magnitude smaller. One immediate consequence as example is that water ice particles mantled by CO${}_2$ ice lose any "sticking advantage." In this case, preferential planetesimal growth attributed to the sticking properties of water ice will be limited to the region between the H${}_2$O ice line and the CO${}_2$ ice line.

References in corpus (5)

• The stickiness of micrometer-sized water-ice particles
• High Velocity Dust Collisions: Forming Planetesimals in a Fragmentation Cascade with Final Accretion
• Macroscopic Dust in Protoplanetary Disks - From Growth to Destruction
• A dearth of small particles in debris disks: An energy-constrained smallest fragment size
• Collisions of solid ice in planetesimal formation

Cited by in corpus (50)

• Observations of Protoplanetary Disk Structures
• The Mass and Size Distribution of Planetesimals Formed by the Streaming Instability. I. The Role of Self-Gravity
• Contacts of Water Ice in Protoplanetary Disks - Laboratory Experiments
• Setting the volatile composition of (exo)planet-building material. Does chemical evolution in disk midplanes matter?
• Dust evolution in protoplanetary discs and the formation of planetesimals. What have we learned from laboratory experiments?
• Transport of CO in Protoplanetary Disks: Consequences of Pebble Formation, Settling, and Radial Drift
• Dust Density Distribution and Imaging Analysis of Different Ice Lines in Protoplanetary Disks
• How planetary growth outperforms migration
• Ice Grain Collisions in Comparison: CO${}_2$, H${}_2$O and their Mixtures
• Nonsticky Ice at the Origin of the Uniformly Polarized Submillimeter Emission from the HL Tau Disk
• Efficient planet formation by pebble accretion in ALMA rings
• Unveiling Dust Aggregate Structure in Protoplanetary Disks by Millimeter-wave Scattering Polarization
• Water delivery by pebble accretion to rocky planets in habitable zones in evolving disks
• Effect of nucleation on icy pebble growth in protoplanetary discs
• Grand challenges in protoplanetary disc modelling
• Carbon depletion observed inside T Tauri inner rims: Formation of icy, kilometer size planetesimals by 1 Myr
• Understanding planet formation using microgravity experiments
• How large are the monomers of dust aggregates in planet-forming disks?: Insights from quantitative optical and near-infrared polarimetry
• X-ray photoevaporation's limited success in the formation of planetesimals by the streaming instability
• Failed Growth at the Bouncing Barrier in Planetesimal Formation
• Drifting inwards in protoplanetary discs II: The effect of water on sticking properties at increasing temperatures
• Rapid Elimination of Small Dust Grains in Molecular Clouds
• Transmission Electron Microscopy Study of the Morphology of Ices Composed of H2O, CO2, and CO on Refractory Grains
• Formation of Comets
• Support for fragile porous dust in a gravitationally self-regulated disk around IM Lup
• The role of pebble fragmentation in planetesimal formation II. Numerical simulations
• Is There a Temperature Limit in Planet Formation at 1000 K?
• Simulating Observations of Ices in Protoplanetary Disks
• Disc population synthesis: Decrease in the solid mass reservoir through pebble drift
• Composition and Size Dependent Sorting in Preplanetary Growth: Seeding the Formation of Mercury-like Planets
• On the stickiness of CO${}_2$ and H${}_2$O ice particles
• Significant interstellar object production by close stellar flybys
• Influences of three-dimensional gas flow induced by protoplanets on pebble accretion --$\mathrm{I}$. shear regime
• Are Pebble Pile Planetesimals Doomed?
• The impact of pre-main sequence stellar evolution on midplane snowline locations and C/O in planet forming discs
• Different degrees of nitrogen and carbon depletion in the warm molecular layers of protoplanetary disks
• Dust grains cannot grow to millimeter sizes in protostellar envelopes
• Collisional Growth and Fragmentation of Dust Aggregates. II. Mass Distribution of Icy Fragments
• Growth of Aggregates with Liquid-Like Ice-Shells in Protoplanetary Discs
• Thermal processing of primordial pebbles in evolving protoplanetary disks
• ARISE: A granular matter experiment on the International Space Station
• The Molecular Composition of Shadowed Protosolar Disk Midplanes beyond the Water Snowline
• Onset of planet formation in the warm inner disk -- Colliding dust aggregates at high temperatures
• Chemistry During the Gas-rich Stage of Planet Formation
• Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks II: Dust Ring Formation Mediated by Backreaction and Fragmentation
• Selective Aggregation Experiments on Planetesimal Formation and Mercury-Like Planets
• Dust ring and gap formation by gas flow induced by low-mass planets embedded in protoplanetary disks $\mathrm{I}$. Steady-state model
• Dust ring and gap formation by gas flow induced by low-mass planets embedded in protoplanetary disks $\mathrm{II}$. Time-dependent model
• Exploring the conditions for forming planetesimals by the streaming instability and planetary systems by pebble accretion
• A Pathway for Collisional Planetesimal Growth in the Ice-Dominant Regions of Protoplanetary Disks