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We investigate the coupling between rock-size solids and gas during theformation of gas giant planets by disk fragmentation in the outer regions ofmassive disks. In this study, we use three-dimensional radiative hydrodynamicssimulations and model solids as a spatial distribution of particles. We assumethat half of the total solid fraction is in small grains and half in largesolids. The former are perfectly entrained with the gas and set the opacity inthe disk, while the latter are allowed to respond to gas drag forces, with theback reaction on the gas taken into account. To explore the maximum effects ofgas-solid interactions, we first consider 10cm-size particles. We then comparethese results to a simulation with 1 km-size particles, which explores thelow-drag regime. We show that (1) disk instability planets have the potentialto form large cores due to aerodynamic capturing of rock-size solids in spiralarms before fragmentation; (2) that temporary clumps can concentrate tens of$M_{\oplus}$ of solids in very localized regions before clump disruption; (3)that the formation of permanent clumps, even in the outer disk, is dependent onthe grain-size distribution, i.e., the opacity; (4) that nonaxisymmetricstructure in the disk can create disk regions that have a solids-to-gas ratiogreater than unity; (5) that the solid distribution may affect thefragmentation process; (6) that proto-gas giants and proto-brown dwarfs canstart as differentiated objects prior to the H$_2$ collapse phase; (7) thatspiral arms in a gravitationally unstable disk are able to stop the inwarddrift of rock-size solids, even redistributing them to larger radii; and, (8)that large solids can form spiral arms that are offset from the gaseous spiralarms. We conclude that planet embryo formation can be strongly affected by thegrowth of solids during the earliest stages of disk accretion.

On The Possibility of Enrichment and Differentiation in Gas Giants During Birth by Disk Instability