TIDESnnv (Tidal Interactions with Dissipation of Energy due to Shear version nvv)

TIDES is a numerical calculation of the perturbations induced on a binary star by its companion.  The code is written in Fortran.  It simultaneously solves  the equations that describe the orbital  motion and the motion of a 3D grid of volume elements that cover the central region of the tidally perturbed star.   This central region, referred to as the core, rotates as a solid body with constant angular velocity  in an inertial reference frame, and its rotation axis is perpendicular to the orbital plane.   The equations of motion  are solved in the reference frame with origin at the center of the primary star and which rotates at the rate of the companion's orbital motion.  They include gravitational,  centrifugal,  Coriolis, gas pressure gradient, and viscous forces. A seventh order Runge-Kutta integrator is used to solve the set of equations. The companion is considered to be a point-mass source and its orbital plane is coplanar with the primary star's equator.  The input is read in from a file. The output includes the angular velocity, the average turbulent viscosity  and energy dissipation rate for each volume element of the grid as well as the total tidal shear energy dissipation rate as a function of orbital phase.