  The low ionization state in parts of a sunspot may play an important role in
its evolution and dynamical state. The cool magnetic interior region of the
sunspot develops a substantial neutral atomic and molecular hydrogen osmotic
pressure which can drive a wind outward from the umbra. Ambipolar diffusion
against the magnetically pinned ionized plasma component can also distort the
umbral magnetic field into a filamentary penumbral structure. This may be
important for explaining the development of the sunspot penumbra and the
Evershed flow. This fractionation process may also be important for the ``First
Ionization Potential'' (FIP) effect seen in the solar wind. In support of this
mechanism we find evidence for such ionization fractionization in UV
observations of molecular hydrogen in a sunspot umbra and penumbra.
