  High sensitivity interstellar scintillation and polarization observations of
PSR~B0656+14 made at three epochs over a year using the Five-hundred-meter
Aperture Spherical radio Telescope (FAST) show that the scattering is dominated
by two different compact regions. We identify the one nearer to the pulsar with
the shell of the Monogem Ring, thereby confirming the association. The other is
probably associated with the Local Bubble. We find that the observed position
angles of the pulsar spin axis and the space velocity are significantly
different, with a separation of $19\fdg3\pm$0\fdg8, inconsistent with a
previously published near-perfect alignment of $1\degr\pm 2\degr$. The two
independent scattering regions are clearly defined in the secondary spectra
which show two strong forward parabolic arcs. The arc curvatures imply that the
scattering screens corresponding to the outer and inner arcs are located
approximately 28~pc from PSR B0656+14 and 185~pc from the Earth, respectively.
Comparison of the observed Doppler profiles with electromagnetic simulations
shows that both scattering regions are mildly anisotropic. For the outer arc,
we estimate the anisotropy $A_R$ to be approximately 1.3, with the scattering
irregularities aligned parallel to the pulsar velocity. For the outer arc, we
compare the observed delay profiles with delay profiles computed from a
theoretical strong-scattering model. Our results suggest that the spatial
spectrum of the scattering irregularities in the Monogem Ring is flatter than
Kolmogorov, but further observations are required to confirm this.
