  We present a new model of the heliospheric interface - the region of the
solar wind interaction with the local interstellar medium. This new model
performs a multi-component treatment of charged particles in the heliosphere.
All charged particles are divided into several co-moving types. The coldest
type, with parameters typical of original solar wind protons, is considered in
the framework of fluid approximation. The hot pickup proton components created
from interstellar H atoms and heliospheric ENAs by charge exchange, electron
impact ionization and photoionization are treated kinetically. The charged
components are considered self-consistently with interstellar H atoms, which
are described kinetically as well. To solve the kinetic equation for H atoms we
use the Monte Carlo method with splitting of trajectories, which allows us 1)
to reduce statistical uncertainties allowing correct interpretation of
observational data, 2) to separate all H atoms in the heliosphere into several
populations depending on the place of their birth and on the type of parent
protons.
