Sticking Properties of Silicates in Planetesimal Formation Revisited

Abstract

In the past, laboratory experiments and theoretical calculations showed a mismatch in derived sticking properties of silicates in the context of planetesimal formation. It has been proposed by Kimura et al. (2015) that this mismatch is due to the value of the surface energy assumed, supposedly correlated to the presence or lack of water layers of different thickness on a grain's surface. We present tensile strength measurements of dust aggregates with different water content here. The results are in support of the suggestion by Kimura et al. (2015). Dry samples show increased strengths by a factor of up to 10 over wet samples. A high value of $\gamma =0.2J/m^2$ likely applies to the dry low pressure conditions of protoplanetary disks and should be used in the future.

References in corpus (4)

• Cohesion of Amorphous Silica Spheres: Toward a Better Understanding of the Coagulation Growth of Silicate Dust Aggregates
• The physics of protoplanetesimal dust agglomerates. VII The low-velocity collision behavior of large dust agglomerates
• Experiments on centimeter-sized dust aggregates and their implications for planetesimal formation
• Experimental study on compression property of regolith analogues

Cited by in corpus (62)

• On the diversity of asymmetries in gapped protoplanetary disks
• How dust fragmentation may be beneficial to planetary growth by pebble accretion
• A Tale of Planet Formation: From Dust to Planets
• Growing and Trapping Pebbles with Fragile Collisions of Particles in Protoplanetary Disks
• The Galilean Satellites Formed Slowly from Pebbles
• Understanding planet formation using microgravity experiments
• The tensile strength of dust aggregates consisting of small elastic grains: Constraints on the size of condensates in protoplanetary disks
• Drifting inwards in protoplanetary discs II: The effect of water on sticking properties at increasing temperatures
• How to make giant planets via pebble accretion
• Millimeter-sized Dust Grains Appear Surviving the Water-sublimating Temperature in the Inner 10 au of the FU Ori Disk
• A bright inner disk and structures in the transition disk around the very low-mass star CIDA 1
• ALMA Observations of the Asymmetric Dust Disk around DM Tau
• Sticky or not sticky? Measurements of the tensile strength of micro-granular organic materials
• Gas accretion damped by dust back-reaction at the snow line
• Cohesion of regolith: Measurements of meteorite powders
• Radial Gradients in Dust-to-Gas Ratio Lead to Preferred Region for Giant Planet Formation
• Towards a population synthesis of discs and planets. II. Confronting disc models and observations at the population level
• Composition and Size Dependent Sorting in Preplanetary Growth: Seeding the Formation of Mercury-like Planets
• Rocky Planetesimal Formation Aided by Organics
• The impact of dynamic pressure bumps on the observational properties of protoplanetary disks
• Self-Induced Dust Traps Around Snow Lines in Protoplanetary Discs
• Dust hot spots at 10 au scales around the Class 0 binary IRAS 16293-2422 A: a departure from the passive irradiation model
• Planetesimal formation around the snow line. II. Dust or pebbles?
• Coagulation Instability in Protoplanetary Disks: A Novel Mechanism Connecting Collisional Growth and Hydrodynamical Clumping of Dust Particles
• The formation of wide exoKuiper belts from migrating dust traps
• Planetesimals in Rarefied Gas: Wind Erosion in Slip Flow
• New growth mechanism of dust grains in protoplanetary disks with magnetically driven disk winds
• Lifting Grains by the Transient Low Pressure in a Martian Dust Devil
• Evolution of dust porosity through coagulation and shattering in the interstellar medium
• Planetesimal formation around the snow line: I. Monte Carlo simulations of silicate dust pile-up in a turbulent disk
• Toward a Population Synthesis of Disks and Planets I. Evolution of Dust with Entrainment in Winds and Radiation Pressure
• Drifting inwards in protoplanetary discs I Sticking of chondritic dust at increasing temperatures
• The impact of dust evolution on the dead zone outer edge in magnetized protoplanetary disks
• Transport, destruction and growth of pebbles in the gas envelope of a protoplanet
• Electrostatic Repulsion of Dust from Planetary Surfaces
• Magnetic disk winds in protoplanetary disks: Description of the model and impact on global disk evolution
• Onset of planet formation in the warm inner disk -- Colliding dust aggregates at high temperatures
• Millimeter emission in photoevaporating disks is determined by early substructures
• Massive Protostellar Disks as a Hot Laboratory of Silicate Grain Evolution
• Evolution of dust grain size distribution and grain porosity in galaxies
• Monte Carlo Simulation of Dust Particles in a Protoplanetary Disk: Crystalline to Amorphous Silicate Ratio in Comets
• Forbidden planetesimals
• The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO): VI. Comparison of Dust Evolution Models to AGE-PRO Observations
• The solar abundance problem and eMSTOs in clusters
• Planetesimal formation via the streaming instability in simulations of infall dominated young disks
• Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks II: Dust Ring Formation Mediated by Backreaction and Fragmentation
• Dust release from cold ring particles as a mechanism of spoke formation in Saturn's rings
• Destruction of eccentric planetesimals by ram pressure and erosion
• ALMA Observations of the Inner Cavity in the Protoplanetary Disk around Sz 84
• The rotational disruption of porous dust aggregates from ab-initio kinematic calculations
• Primordial porous structure of chondrite parent bodies due to self-gravity
• Probing Inner-Edge of Dead Zones in Protoplanetary Disks with ALMA and Next Generation Very Large Array
• Clusters of tribocharged dust aggregates as pebbles in protoplanetary disks
• Gas Phase Ions in Protoplanetary Disks from Collisions of Solids
• A "no-drift" runaway pile-up of pebbles in protoplanetary disks II. Characteristics of the resulting planetesimal belt
• Revisiting sticking property of submillimetre-sized aggregates
• The Dissolution of Planetesimals in Electrostatic Fields
• A multiwavelength analysis of the spiral arms in the protoplanetary disk around WaOph 6
• The Impact of Silicate Grain Coagulation on Millimeter Emission from Massive Protostellar Disks
• Thermally driven spontaneous dust accumulation in the inner regions of protoplanetary disks
• Evading the dust fragmentation barrier with the streaming instability in protoplanetary disks
• Gas Phase Ion Species Released During Grain Collisions: Implications For Protoplanetary Disks