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The streaming instability, a promising mechanism to drive planetesimalformation in dusty protoplanetary discs, relies on aerodynamic drag naturallyinduced by the background radial pressure gradient. This gradient should varyin disks, but its effect on the streaming instability has not been sufficientlyexplored. For this purpose, we use numerical simulations of an unstratifieddisc to study the non-linear saturation of the streaming instability withmono-disperse dust particles and survey a wide range of gradients for twodistinct combinations of the particle stopping time and the dust-to-gas massratio. As the gradient increases, we find most kinematic and morphologicalproperties increase but not always in linear proportion. The densitydistributions of tightly-coupled particles are insensitive to the gradientwhereas marginally-coupled particles tend to concentrate by more than an orderof magnitude as the gradient decreases. Moreover, dust-gas vortices fortightly-coupled particles shrink as the gradient decreases, and we note higherresolutions are required to trigger the instability in this case. In addition,we find various properties at saturation that depend on the gradient may beobservable and may help reconstruct models of observed discs dominated bystreaming turbulence. In general, increased dust diffusion from strongergradients can lower the concentration of dust filaments and can explain thehigher solid abundances needed to trigger strong particle clumping and thereduced planetesimal formation efficiency previously found invertically-stratified simulations.

Dust-gas dynamics driven by the streaming instability with various pressure gradients