Drifting inwards in protoplanetary discs I Sticking of chondritic dust at increasing temperatures

Abstract

Sticking properties rule the early phases of pebble growth in protoplanetary discs in which grains regularly travel from cold, water-rich regions to the warm inner part. This drift affects composition, grain size, morphology, and water content as grains experience ever higher temperatures. In this study we tempered chondritic dust under vacuum up to 1400 K. Afterwards, we measured the splitting tensile strength of millimetre-sized dust aggregates. The deduced effective surface energy starts out as ${\gamma }_e=0.07J/{\mathrm{m}}^2$. This value is dominated by abundant iron-oxides as measured by Mössbauer spectroscopy. Up to 1250 K, ${\gamma }_e$ continuously decreases by up to a factor five. Olivines dominate at higher temperature. Beyond 1300 K dust grains significantly grow in size. The ${\gamma }_e$ no longer decreases but the large grain size restricts the capability of growing aggregates. Beyond 1400 K aggregation is no longer possible. Overall, under the conditions probed, the stability of dust pebbles would decrease towards the star. In view of a minimum aggregate size required to trigger drag instabilities it becomes increasingly harder to seed planetesimal formation closer to a star.

References in corpus (19)

• Streaming Instabilities in Protoplanetary Disks
• Fluffy dust forms icy planetesimals by static compression
• On the Location of the Snow Line in a Protoplanetary Disk
• Fossilized condensation lines in the Solar System protoplanetary disk
• Contacts of Water Ice in Protoplanetary Disks - Laboratory Experiments
• Cohesion of Amorphous Silica Spheres: Toward a Better Understanding of the Coagulation Growth of Silicate Dust Aggregates
• Sticking Properties of Silicates in Planetesimal Formation Revisited
• Planet formation and migration near the silicate sublimation front in protoplanetary disks
• Effect of nucleation on icy pebble growth in protoplanetary discs
• Subsolar Al/Si and Mg/Si ratios of non-carbonaceous chondrites reveal planetesimal formation during early condensation in the protoplanetary disk
• Curved walls: Grain growth, settling, and composition patterns in T Tauri disk dust sublimation fronts
• Experiments on centimeter-sized dust aggregates and their implications for planetesimal formation
• Saltation under Martian Gravity and its Influence on the Global Dust Distribution
• Micrometer-Sized Water Ice Particles for Planetary Science Experiments: Influence of Surface Structure on Collisional Properties
• Is There a Temperature Limit in Planet Formation at 1000 K?
• Experimental study on compression property of regolith analogues
• Self-Induced Dust Traps Around Snow Lines in Protoplanetary Discs
• Constraints on Compound Chondrule Formation from Laboratory High-Temperature Collisions
• Onset of planet formation in the warm inner disk -- Colliding dust aggregates at high temperatures

Cited by in corpus (5)

• Distribution of solids in the rings of the HD 163296 disk: a multiwavelength study
• Drifting inwards in protoplanetary discs II: The effect of water on sticking properties at increasing temperatures
• Observation of bottom-up formation for charged grain aggregates related to pre-planetary evolution beyond the bouncing barrier
• Presolar grain dynamics: creating nucleosynthetic variations through a combination of drag and viscous evolution
• The rotational disruption of porous dust aggregates from ab-initio kinematic calculations