  Shortfalls in cosmic ray (CR) propagation models obscure the CR sources and
acceleration mechanisms. This problem became particularly obvious after the
Fermi, Pamela, and AMS-02 have discovered the electron/positron and $p/$He
spectral anomalies. Most of the CR models use diffusive propagation that is
inaccurate for weakly scattered energetic particles. So, some parts of the
spectra affected by the heliospheric modulation, for example, cannot be
interpreted. I discuss and adopt an exact solution of the Fokker-Planck
equation arXiv1610.01584, which gives a complete description of a ballistic,
diffusive and transdiffusive (intermediate between the first two) propagation
regimes. I derive a simplified version of an exact Fokker-Planck propagator
that can easily be employed in place of the Gaussian propagator, currently used
in major Solar modulation and other CR transport models.
