  Recently, we correlated the inferred structure of the solar chromospheric
plasma topography with solar wind velocity and composition data measured at
1AU. We now offer a physical justification of these relationships and present
initial results of a empirical prediction model based on them. While still
limited by the fundamentally complex physics behind the origins of the solar
wind and how its structure develops in the magnetic photosphere and expands
into the heliosphere, our model provides a near continuous range of solar wind
speeds and composition quantities that are simply estimated from the inferred
structure of the chromosphere. We suggest that the derived quantities may
provide input to other, more sophisticated, prediction tools or models such as
those to study Coronal Mass Ejections (CME) propagation and Solar Energetic
Particle (SEP) generation.
