The interface between the outer heliosphere and the inner lism:
  Morphology of the local interstellar cloud, its hydrogen hole, stromgren
  shells, and $^{60}$Fe accretion
  We describe the interface between the outer heliosphere and the local
interstellar medium (LISM) surrounding the Sun. The components of the inner
LISM are the four partially ionized clouds [the Local Interstellar Cloud (LIC),
G cloud, Blue cloud, and Aql cloud] that are in contact with the outer
heliosphere, and ionized gas produced by EUV radiation primarily from
$\epsilon$~CMa. We construct the three-dimensional shape of the LIC based on
interstellar line absorption along 62 sightlines and show that in the direction
of $\epsilon$~CMa, $\beta$~CMa, and Sirius~B the neutral hydrogen column
density from the center of the LIC is a minimum. We call this region the
``hydrogen hole''. In this direction, the presence of Blue cloud absorption and
the absence of LIC absorption can be simply explained by the Blue cloud lying
just outside of the heliosphere. We propose that the outer edge of the Blue
cloud is a Str\"omgren shell driven toward the heliosphere by high pressures in
the H~II region. We find that the vectors of neutral and ionized helium flowing
through the heliosphere are inconsistent with the LIC flow vector, and that the
nearby intercloud gas is consistent with ionization by $\epsilon$~CMa and other
stellar sources without requiring additional sources of ionization or million
degree plasma. In the upwind direction, the heliosphere is passing through an
environment of several LISM clouds, which may explain the recent influx of
interstellar grains containing $^{60}$Fe from supernova ejecta measured in
Antarctica snow.
