  The diversity of the structures recently observed in protoplanetary discs
(PPDs) with the new generation of high-resolution instruments have made more
acute the challenging questions that planet-formation models must answer. The
challenge is in the theoretical side but also in the numerical one with the
need to significantly improve the performances of the codes and to stretch the
limit of PPD simulations. Multi-physics, fast, accurate, high-resolution,
modular, and reliable 3D codes are needed to explore the mechanisms at work in
PPDs and to try explaining the observed features. We present RoSSBi3D the 3D
extension of the 2D code Rotating-System Simulations for Bi-fluids (RoSSBi)
which was specifically developed to study the evolution of PPDs. This is a new
code, even if based on the 2D version, that we describe in detail explaining
its architecture and specificity but also its performances against test cases.
This grid-based, FORTRAN code solves the fully compressible inviscid
continuity, Euler and energy conservation equations for an ideal gas in
non-homentropic conditions and for pressureless particles in a fluid
approximation. It is a finite volume code which is second order in time and
accounts for discontinuities thanks to an exact Riemann solver. The spatial
scheme accounts for the equilibrium solution and is improved thanks to
parabolic interpolation. The code is developed in 3D and structured for
high-performance parallelism. The optimised version of the code works on
high-performance computers with excellent scalability. We checked its
reliability against a 2D analogue of the sod shock tube test and a series of
tests. We release this code under the terms of the CeCILL2 Licence and make it
publicly available.

Earth and Planetary Astrophysics;Instrumentation and Methods for Astrophysics;Computational Physics