This thesis examines a proposed source of the slow solar wind at the boundaries of active regions. It shows the time variability observed in the wind can be produced by time-variable heating in such regions. To understand how these structures contribute to observed outflows, we adapt a two-fluid hydrodynamic model of the solar corona. Adjusting model parameters within their physical bounds allows us to reproduce the expected values for the slow wind and gain a better understanding of the energy deposition along coronal flux tubes.

We use forward models to compare with observations from the Extreme Ultraviolet Imaging Spectrometer aboard Hinode. Non-thermal line broadening and Doppler shifts are calculated for quantitative comparisons. The simulations including non-equilibrium ionization indicate equilibrium ionization cannot be assumed in many cases. Successful reproduction of remote sensing observations leaves us optimistic about future comparisons with in situ measurements from the space missions Solar Probe+ and Solar Orbiter.