  Here we present CAFein, a new computational tool for investigating radiative
dissipation of dynamic tides in close binaries and of non-adiabatic, non-radial
stellar oscillations in isolated stars in the linear regime. For the latter,
CAFein computes the non-adiabatic eigenfrequencies and eigenfunctions of
detailed stellar models. The code is based on the so-called Riccati method, a
numerical algorithm that has been successfully applied to a variety of stellar
pulsators, and which doesn't suffer of the major drawbacks of commonly used
shooting and relaxation schemes. Here we present an extension of the Riccati
method to investigate dynamic tides in close binaries. We demonstrate CAFein's
capabilities as a stellar pulsation code both in the adiabatic and
non-adiabatic regime, by reproducing previously published eigenfrequencies of a
polytrope, and by successfully identifying the unstable modes of a stellar
model in the $\beta$ Cephei/SPB region of the Hertzsprung-Russell diagram.
Finally, we verify CAFein's behavior in the dynamic tides regime by
investigating the effects of dynamic tides on the eigenfunctions and orbital
and spin evolution of massive Main Sequence stars in eccentric binaries, and of
hot Jupiter host stars. The plethora of asteroseismic data provided by the
NASA's Kepler satellite, some of which include the direct detection of tidally
excited stellar oscillations, make CAFein quite timely. Furthermore, the
increasing number of observed short-period detached double white dwarfs (WD)
and the observed orbital decay in the tightest of such binaries open up a new
possibility of investigating WD interiors through the effects of tides on their
orbital evolution
