Making the Planetary Material Diversity During the Early Assembling of the Solar System

Abstract

Chondritic meteorites, the building blocks of terrestrial planets, are made of an out-of-equilibrium assemblage of solids formed at high and low temperatures, either in our Solar system or previous generations of stars. This was considered for decades to result from large scale transport processes in the Sun's isolated accretion disk. However, mounting evidences suggest that refractory inclusions in chondrites formed contemporaneously with the disk building. Here we numerically investigate, using a 1D model and several physical and chemical processes, the formation and transport of rocky materials during the collapse of the Sun's parent cloud and the consequent Solar Nebula assembling. The interplay between the cloud collapse, the dynamics of gas and dust, vaporization, recondensation and thermal processing of different species in the disk, results in a local mixing of solids with different thermal histories. Moreover, our results also explains the overabundance of refractory materials far from the Sun and their short formation timescales, during the first tens of kyr of the Sun, corresponding to class 0-I, opening new windows into the origin of the compositional diversity of chondrites.

arXiv commentReceived on 13/08/2018, accepted 24/10/2018. Astrophysical Journal Letters

References in corpus (20)

• The chemical composition of the Sun
• Protoplanetary Disks and Their Evolution
• A simple model for the evolution of the dust population in protoplanetary disks
• Rosseland and Planck Mean Opacities for Protoplanetary Discs
• Evolution of protoplanetary disks: Constraints from DM Tauri and GM Aurigae
• Close-in planetesimal formation by pile-up of drifting pebbles
• Long-term Evolution of Protostellar and Protoplanetary Disks. II. Layered Accretion with Infall
• 2-D simulations of FU Orionis disk outbursts
• Dead Zone Accretion Flows in Protostellar Disks
• Magnetically self-regulated formation of early protoplanetary discs
• Protoplanetary Disks in $\rho$ Ophiuchus as Seen From ALMA
• New composite models of partially ionized protoplanetary disks
• The Envelope and Embedded Disk around the Class 0 Protostar L1157-mm: Dual-wavelength Interferometric Observations and Modeling
• Crystalline silicates as a probe of disk formation history
• From Birth to Death of Protoplanetary Disks: Modeling Their Formation, Evolution, and Dispersal
• Radial transport of refractory inclusions and their preservation in the dead zone
• Coagulation of small grains in disks: the influence of residual infall and initial small-grain content
• Trapping planets in an evolving protoplanetary disk: preferred time, locations and planet mass
• The effect of the regular solution model in the condensation of protoplanetary dust
• Importance of thermal diffusion in the gravo-magnetic limit cycle

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• Bifurcation of planetary building blocks during Solar System formation
• Contemporary formation of early solar system planetesimals at two distinct radial locations
• Elemental and isotopic variability in solar system materials by mixing and processing of primordial disk reservoirs
• Early evolution of the solar accretion disk inferred from Cr-Ti-O isotopes in individual chondrules
• The origin of s-process isotope heterogeneity in the solar protoplanetary disk
• Origin of hydrogen isotopic variations in chondritic water and organics
• Nucleation and growth of iron pebbles explains the formation of iron-rich planets akin to Mercury
• Fingerprints of the protosolar cloud collapse in the Solar System II: Nucleosynthetic anomalies in meteorites
• Formation and evolution of a protoplanetary disk: combining observations, simulations and cosmochemical constraints
• Forming pressure-traps at the snow-line to isolate isotopic reservoirs in the absence of a planet
• Gravitoviscous protoplanetary disks with a dust component. III. Evolution of gas, dust, and pebbles
• An inflationary disk phase to explain extended protoplanetary dust disks
• Fingerprints of the protosolar cloud collapse in the Solar System I: Distribution of presolar short-lived ${}^{26}$Al
• Meteorite petrology versus genetics: Toward a unified binominal classification
• Comparison between core-collapse supernova nucleosynthesis and meteoric stardust grains: investigating magnesium, aluminium, and chromium
• Fast formation of large ice pebbles after FU Orionis outbursts
• Dynamic evolution of major element chemistry in protoplanetary disks and its implications for chondrite formation
• Spatially resolving the chemical composition of the planet building blocks
• Non-equilibrium condensation of the first Solar System solids
• Numerical Insights into Disk Accretion, Eccentricity, and Kinematics in the Class 0 phase
• Protoplanetary disk formation from the collapse of a prestellar core