The Earth.s electromagnetic and energy particle environment are heavily influenced by solar emissions. The two major mechanisms of energy transfer at the ionosphere are particle precipitation and energy in the electromagnetic fields or Poynting flux. Because aerodynamic drag on satellites increases as Earth.s atmosphere heats, there is a strong need to determine appropriate datasets required to specify and forecast the energy input into the system. For more than a dozen cases identified by Air Force Space Command, we have calculated Poynting flux from the DMSP F15satellite ion drift and magnetometer data. We compare these calculations with particle energy data from DMSP particle detectors, thermospheric density enhancements from the GRACE and CHAMP satellites, as well as with ACE solar wind parameters, and ground and space based indices. Many of the AFSPC events are associated with solar wind shocks driven by coronal mass ejections. We find that unexpectedly large values of Poynting flux occur during intervals of northward IMF and/or in the presence of large in-the-ecliptic components of the IMF (BX and BY) and in the dayside high-latitude region. When such conditions are long-lived, substantial energy flows into the high latitude atmosphere that remains largely undetected by models. We are in the process of comparing these results with various models, e.g. Weimer Joule Heat, AMIE, and magnetospheric GCMs.