Recent observations have revealed that protoplanetary discs often exhibit
cavities and azimuthal asymmetries such as dust traps and clumps. The presence
of a stellar binary system in the inner disc regions has been proposed to
explain the formation of these structures. Here, we study the dust and gas
dynamics in circumbinary discs around eccentric and inclined binaries. This is
done through two-fluid simulations of circumbinary discs, considering different
values of the binary eccentricity and inclination. We find that two kinds of
dust structures can form in the disc: a single horseshoe-shaped clump, on top
of a similar gaseous over-density; or numerous clumps, distributed along the
inner disc rim. The latter features form through the complex interplay between
the dust particles and the gaseous spirals caused by the binary. All these
clumps survive between one and several tens of orbital periods at the feature
location. We show that their evolution strongly depends on the gas-dust
coupling and the binary parameters. Interestingly, these asymmetric features
could in principle be used to infer or constrain the orbital parameters of a
stellar companion - potentially unseen - inside the inner disc cavity. Finally,
we apply our findings to the disc around AB Aurigae.Comment: 12 pages, 13 figures, accepted for publication in MNRA
