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Our previous linear analysis presents a new instability driven by dustcoagulation in protoplanetary disks. The coagulation instability has thepotential to concentrate dust grains into rings and assist dust coagulation andplanetesimal formation. In this series of papers, we perform numericalsimulations and investigate nonlinear outcome of coagulation instability. Inthis paper (Paper I), we first conduct local simulations to demonstrate theexistence of coagulation instability. Linear growth observed in the simulationsis in good agreement with the previous linear analysis. We next conductradially global simulations to demonstrate that coagulation instabilitydevelops during the inside-out disk evolution due to dust growth. To isolatethe various effects on dust concentration and growth, we neglect effects ofbackreaction to a gas disk and dust fragmentation in Paper I. This simplifiedsimulation shows that either of backreaction or fragmentation is notprerequisite for local dust concentration via the instability. In most runswith weak turbulence, dust concentration via coagulation instability overcomesdust depletion due to radial drift, leading to the formation of multiple dustrings. The nonlinear development of coagulation instability also acceleratesdust growth, and the dimensionless stopping time $\tau_{\mathrm{s}}$ reachesunity even at outer radii (>10 au). Therefore, coagulation instability is onepromising process to retain dust grains and to accelerate dust growth beyondthe drift barrier.

astrophysical journal/the astrophysical journal

Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks I:  First Numerical Study of Accelerated Dust Growth and Dust Concentration at  Outer Radii