An analysis of polar solar wind proton flux upper limits derived by using Saito's coronal density model shows that in the absence of significant heating beyond 2Rs the flux of protons at high heliographic latitudes should be less than that normally observed in the ecliptic at 1 AU by at least a factor of 4--10. If instead, the polar density values tabulated by Allen are used, then the calculated upper limit proton flux is consistent with that observed in structure-free high-speed regions at the orbit of the earth. Implications of Saito's coronal density model on the reion in the intrmediate corona accessible to exploration by using measurements of solar wind heavy ions at 1 AU were also determined. It is shown that solar wind heavy ion observations at high heliographic latitudes allow a determination of the electron temperature at heights which bracket the nominal location of the coronal temperature maximum. Heavy ion observations should thus provide information concerning the magnitude and extent of mechanical dissipation, as well as details of the solar wind expansion, in the intermediate corona.