Probing the Protosolar Disk Using Dust Filtering at Gaps in the Early Solar System

Abstract

Jupiter and Saturn formed early, before the gas disk dispersed. The presence of gap-opening planets affects the dynamics of the gas and embedded solids and halts the inward drift of grains above a certain size. A drift barrier can explain the absence of calcium aluminium rich inclusions (CAIs) in chondrites originating from parent bodies that accreted in the inner solar system. Employing an interdisciplinary approach, we use a $\mu$-X-Ray-fluorescence scanner to search for large CAIs and a scanning electron microscope to search for small CAIs in the ordinary chondrite NWA 5697. We carry out long-term, two-dimensional simulations including gas, dust, and planets to characterize the transport of grains within the viscous $\alpha$-disk framework exploring the scenarios of a stand-alone Jupiter, Jupiter and Saturn \textit{in situ}, or Jupiter and Saturn in a 3:2 resonance. In each case, we find a critical grain size above which drift is halted as a function of the physical conditions in the disk. From the laboratory search we find four CAIs with a largest size of $\approx$200$\mu$m. \Combining models and data, we provide an estimate for the upper limit of the $\alpha$-viscosity and the surface density at the location of Jupiter, using reasonable assumptions about the stellar accretion rate during inward transport of CAIs, and assuming angular momentum transport to happen exclusively through viscous effects. Moreover, we find that the compound gap structure in the presence of Saturn in a 3:2 resonance favors inward transport of grains larger than CAIs currently detected in ordinary chondrites.

16 pages, 10 figures, updated to match published version in Astrophysical Journal

References in corpus (16)

• The NumPy array: a structure for efficient numerical computation
• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• Building Terrestrial Planets
• A comparative study of disc-planet interaction
• A Three-Dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk using DCO${}^{+}$
• Lupus disks with faint CO isotopologues: low gas/dust or large carbon depletion?
• The Migration of Gap-Opening Planets is not Locked to Viscous Disk Evolution
• Migration of massive planets in accreting disks
• Treating gravity in thin disk simulations
• Infall-Driven Protostellar Accretion and the Solution to the Luminosity Problem
• Episodic accretion: the interplay of infall and disc instabilities
• Particle dynamics in discs with turbulence generated by the vertical shear instability
• Explaining the luminosity spread in young clusters: proto and pre-main sequence stellar evolution in a molecular cloud environment
• Measuring protoplanetary disk gas surface density profiles with ALMA
• A Unified Framework for Producing CAI Melting, Wark-Lovering Rims and Bowl-Shaped CAIs
• Circumstellar dust distribution in systems with two planets in resonance

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• Assessment of Cr isotopic heterogeneities of volatile-rich asteroids based on multiple planet formation models
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