  Recent high-spatial-resolution observations have revealed dust substructures
in protoplanetary disks such as rings and gaps, which do not always correlate
with gas. Because radial gas flow induced by low-mass, non-gas-gap-opening
planets could affect the radial drift of dust, it potentially forms these dust
substructures in disks. We investigate the potential of gas flow induced by
low-mass planets to sculpt the rings and gaps in the dust profiles. We first
perform three-dimensional hydrodynamical simulations, which resolve the local
gas flow past a planet. We then calculate the trajectories of dust influenced
by the planet-induced gas flow. Finally, we compute the steady-state dust
surface density by incorporating the influences of the planet-induced gas flow
into a one-dimensional dust advection-diffusion model. The outflow of the gas
toward the outside of the planetary orbit inhibits the radial drift of dust,
leading to dust accumulation (the dust ring). The outflow toward the inside of
the planetary orbit enhances the inward drift of dust, causing dust depletion
around the planetary orbit (the dust gap). Under weak turbulence ($\alpha_{\rm
diff}\lesssim10^{-4}$, where $\alpha_{\rm diff}$ is the turbulence strength
parameter), the gas flow induced by the planet with $\gtrsim1\,M_{\oplus}$
(Earth mass) generates the dust ring and gap in the distribution of small dust
grains ($\lesssim1$ cm) with the radial extent of $\sim1\text{--}10$ times gas
scale height around the planetary orbit without creating a gas gap and pressure
bump. The gas flow induced by low-mass, non-gas-gap-opening planets can be
considered a possible origin of the observed dust substructures in disks. Our
results may be helpful to explain the disks whose dust substructures were found
not to correlate with those of the gas.
