  Stellar binaries represent a substantial fraction of stellar systems,
especially among young stellar objects. Accordingly, binaries play an important
role in setting the architecture of a large number of protoplanetary discs.
Binaries in coplanar and polar orientations with respect to the circumbinary
disc are stable configurations and could induce non-axisymmetric structures in
the dust and gas distributions. In this work, we suggest that the structures
shown in the central region of the protoplanetary disc HD 169142 are produced
by the presence of an inner stellar binary and a circumbinary (P-type) planet.
We find that a companion with a mass-ratio of 0.1, semi-major axis of 9.9 au,
eccentricity of 0.2, and inclination of 90{\deg}, together with a 2 Jupiter
Mass coplanar planet on a circular orbit at 45 au reproduce the structures at
the innermost ring observed at 1.3 mm and the shape of spiral features in
scattered light observations. The model predicts changes in the disc's dust
structure, and star's astrometric parameters, which would allow testing its
veracity by monitoring this system over the next 20 years.
