  Solar Wind Charge-Exchange (SWCX) emission is present in every X-ray
observation of an astrophysical object. The emission is problematic when one
cannot remove the foreground by the simultaneous measurement of a nearby field.
SWCX emission is a serious impediment to the study of the diffuse hot ISM,
including the Galactic halo, as its contribution to diagnostic emission lines
is temporally variable. Modeling the SWCX emission, in order to remove it from
our observations, has proven to be more difficult than originally anticipated.
This work reviews our current understanding of SWCX emission, with special
attention to all of the components required for future modeling tools. Since,
in the absence of such a tool, observing programs can still be constructed to
minimize the effect of SWCX, mitigation strategies are discussed. Although some
aspects of SWCX will be very difficult to characterize, progress continues on
many fronts.
