  We introduce a new hybrid method to perform high-resolution tidal disruption
simulations, at arbitrary orbits. An SPH code is used to simulate tidal
disruptions only in the immediate spatial domain of the star, namely, where the
tidal forces dominate over gravity, and then during the fragmentation phase in
which the emerging tidal stream may collapse under its own gravity to form
fragments. Following each hydrodynamical simulation, an analytical treatment is
then applied to instantaneously transfer each fragment back to the tidal sphere
for its subsequent disruption, in an iterative process. We validate the hybrid
model by comparing it to both an analytical impulse approximation model of
single tidal disruptions, as well as full-scale SPH simulations spanning the
entire disc formation. The hybrid simulations are essentially indistinguishable
from the full-scale SPH simulations, while computationally outperforming their
counterparts by orders of magnitude. Thereby our new hybrid approach uniquely
enables us to follow the long-term formation and continuous tidal disruption of
the planet/planetesimal debris, without the resolution and orbital
configuration limitation of previous studies. In addition, we describe a
variety of future directions and applications for our hybrid model, which is in
principle applicable to any star, not merely white dwarfs
