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The icy satellites around Jupiter are considered to have formed in acircumplanetary disk. While previous models focused on the formation ofsatellites starting from satellitesimals, the question of how satellitesimalsform from smaller dust particles has not been addressed so far. In this work,we study the possibility that satellitesimals form in situ in a circumplanetarydisk. We calculate the radial distribution of the surface density andrepresentative size of icy dust particles that grow by colliding with eachother and drift toward the central planet in a steady circumplanetary disk witha continuous supply of gas and dust from the parent protoplanetary disk. Theradial drift barrier is overcome if the ratio of the dust to gas accretionrates onto the circumplanetary disk,$\dot{M}_{\mathrm{d}}/\dot{M}_{\mathrm{g}}$, is high and the strength ofturbulence, $\alpha$, is not too low. The collision velocity is lower than thecritical velocity of fragmentation when $\alpha$ is low. Taken together, wefind that the conditions for satellitesimal formation via dust coagulation aregiven by $\dot{M}_{\mathrm{d}}/\dot{M}_{\mathrm{g}}\ge1$ and$10^{-4}\le\alpha<10^{-2}$. The former condition is generally difficult toachieve, suggesting that the in-situ satellitesimal formation via particlesticking is viable only under an extreme condition. We also show that neithersatellitesimal formation via the collisional growth of porous aggregates norvia streaming instability is viable as long as$\dot{M}_{\mathrm{d}}/\dot{M}_{\mathrm{g}}$ is low.

Satellitesimal Formation via Collisional Dust Growth in Steady Circumplanetary Disks