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Spiral arms are distinctive features of many circumstellar disks, observed inscattered light, which traces the disk surface, millimeter dust emission, whichprobes the disk midplane, as well as molecular emission. The two leadingexplanations for spirals are wakes generated by a massive planet and thedensity waves excited by disk self-gravity. We use stratified 3D hydrodynamicshearing-box simulations including dust particles and disk self-gravity toinvestigate how gas and dust spirals in a self-gravitating disk depend on thesimulation size, the cooling efficiency, and the aerodynamics properties ofparticles. We find that opening angles of spirals are universal ($\sim10^o$),and not significantly affected by the size of the computational domain, thecooling time, or the particle size. In simulations with the biggest domain, thespirals in the gaseous disk become slightly more open with a higher coolingefficiency. Small dust follows the gaseous spirals very well, whileintermediate-sized dust with dimensionless stopping time $(\mathrm{St})$ closeto 1 concentrates to the spirals more and shows stronger spirals. However,large dust with $\mathrm{St} > 1$ also shows spirals, which is different fromsome previous simulations. We identify that this is due to the gravity from thegas to the dust component. We show that when $\mathrm{St} \gtrsim Q$, thegravitational force from the gaseous spirals to the dust particles becomesstronger than the particles' aerodynamic drag force, so that the gassignificantly affects these large particles through gravitational interaction.This has important implications for both spiral observations and planetesimalformation/dynamics.

Particle Dynamics in 3D Self-gravitating Disks I: Spirals