  Recent ALMA observations of the protoplanetary disc around HD~169142 reveal a
peculiar structure made of concentric dusty rings: a main ring at $\sim$20 au,
a triple system of rings at $\sim 55-75$ au in millimetric continuum emission
and a perturbed gas surface density from the $^{12}$CO,$^{13}$CO and
C$^{18}$O$(J=2-1)$ surface brightness profile. In this Letter, we perform
three-dimensional numerical simulations and radiative transfer modeling
exploring the possibility that two giant planets interacting with the disc and
orbiting in resonant locking can be responsible for the origin of the observed
dust inner rings structure. We find that in this configuration the dust
structure is actually long lived while the gas mass of the disc is accreted
onto the star and the giant planets, emptying the inner region. In addition, we
also find that the innermost planet is located at the inner edge of the dust
ring, and can accrete mass from the disc, generating a signature in the dust
ring shape that can be observed in mm ALMA observations.
