Ice Grain Collisions in Comparison: CO${}_2$, H${}_2$O and their Mixtures

Abstract

Collisions of ice particles play an important role in the formation of planetesimals and comets. In recent work we showed, that CO${}_2$ ice behaves like silicates in collisions. The resulting assumption was that it should therefore stick less efficiently than H${}_2$O ice. Within this paper a quantification of the latter is presented. We used the same experimental setup to study collisions of pure CO${}_2$ ice, pure water ice and 50\% mixtures by mass between CO${}_2$ and water at 80K, 1 mbar and an average particle size of $\sim 90\mu$m. The results show a strong increase of the threshold velocity between sticking and bouncing with increasing water content. This supports the idea that water ice is favorable for early growth phases of planets in a zone within the H${}_2$O and the CO${}_2$ iceline.

References in corpus (6)

• The stickiness of micrometer-sized water-ice particles
• Dust coagulation in protoplanetary disks: porosity matters
• Comets formed in solar-nebula instabilities! -- An experimental and modeling attempt to relate the activity of comets to their formation process (corrigendum included)
• Microgravity experiments on the collisional behavior of Saturnian ring particles
• The measured compositions of Uranus and Neptune from their formation on the CO iceline
• A dearth of small particles in debris disks: An energy-constrained smallest fragment size

Cited by in corpus (36)

• Contacts of Water Ice in Protoplanetary Disks - Laboratory Experiments
• Dust Density Distribution and Imaging Analysis of Different Ice Lines in Protoplanetary Disks
• Nonsticky Ice at the Origin of the Uniformly Polarized Submillimeter Emission from the HL Tau Disk
• A fading radius valley towards M-dwarfs, a persistent density valley across stellar types
• Growing and Trapping Pebbles with Fragile Collisions of Particles in Protoplanetary Disks
• 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
• Micrometer-Sized Water Ice Particles for Planetary Science Experiments: Influence of Surface Structure on Collisional Properties
• Support for fragile porous dust in a gravitationally self-regulated disk around IM Lup
• Is There a Temperature Limit in Planet Formation at 1000 K?
• Disc population synthesis: Decrease in the solid mass reservoir through pebble drift
• Self-Induced Dust Traps Around Snow Lines in Protoplanetary Discs
• On the stickiness of CO${}_2$ and H${}_2$O ice particles
• Pebble accretion in class 0/I YSOs as a possible pathway for early planet formation
• Influences of three-dimensional gas flow induced by protoplanets on pebble accretion --$\mathrm{I}$. shear regime
• Thermal conductivity and coordination number of compressed dust aggregates
• The formation of wide exoKuiper belts from migrating dust traps
• Discovery of Line Pressure Broadening and Direct Constraint on Gas Surface Density in a Protoplanetary Disk
• Tracking Dust Grains During Transport and Growth in Protoplanetary Disks
• Different degrees of nitrogen and carbon depletion in the warm molecular layers of protoplanetary disks
• 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
• Compaction during fragmentation and bouncing produces realistic dust grain porosities in protoplanetary discs
• ARISE: A granular matter experiment on the International Space Station
• The Molecular Composition of Shadowed Protosolar Disk Midplanes beyond the Water Snowline
• Global Modeling of Nebulae With Particle Growth, Drift, and Evaporation Fronts. II. The Influence of Porosity on Solids Evolution
• Impacts of viscous dissipation on collisional growth and fragmentation of dust aggregates
• Threshold velocity for collisional growth of porous dust aggregates consisting of cohesive frictionless spheres
• Global Modeling of Nebulae With Particle Growth, Drift, and Evaporation Fronts. III. Redistribution of Refractories and Volatiles
• Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks II: Dust Ring Formation Mediated by Backreaction and Fragmentation
• 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
• Giant planet formation via pebble accretion across different stellar masses
• Models and Observational Predictions of Dust Traps in Protoplanetary Discs
• A Pathway for Collisional Planetesimal Growth in the Ice-Dominant Regions of Protoplanetary Disks