Mercury-T calculates the evolution of semi-major axis, eccentricity, inclination, rotation period and obliquity of the planets as well as the rotation period evolution of the host body; it is based on the N-body code Mercury (Chambers 1999, ascl:1201.008). It is flexible, allowing computation of the tidal evolution of systems orbiting any non-evolving object (if its mass, radius, dissipation factor and rotation period are known), but also evolving brown dwarfs (BDs) of mass between 0.01 and 0.08 M⊙, an evolving M-dwarf of 0.1 M⊙, an evolving Sun-like star, and an evolving Jupiter.

The N-body code TIDYMESS (TIdal DYnamics of Multi-body ExtraSolar Systems) can describe the mass distribution of each body its inertia tensor and directly and self-consistently integrates orbit, spin, and inertia tensors. It manages the deformation of a body follows the tidal Creep model and includes the centrifugal force and tidal force. Written in C++, TIDYMESS is available as a standalone package and also through the AMUSE framework (ascl:1107.007).

RheoVolution (Rheology evolution) numerically investigates the dynamical evolution of deformable celestial bodies. Each body can be considered as a point mass, a rigid body, or a deformable body, where both the centrifugal and tidal forces can be set independently, and a permanent deformation (triaxiality) can also be assigned to each body. RheoVolution uses the GNU Scientific Library (GSL) for some tasks, such as numerical integration of ODEs, matrix diagonalization, and linear systems solving, and the package contains a Makefile to compile and help run the code.