  We present Cloudy modeling of infrared emission lines in the Wolf-Rayet (WR)
nebula N76 caused by one of the most luminous and hottest WR stars in the low
metallicity Small Magellanic Cloud. We use spatially resolved mid-infrared
Spitzer/IRS and far-infrared Herschel/PACS spectroscopy to establish the
physical conditions of the ionized gas. The spatially resolved distribution of
the emission allows us to constrain properties much more accurately than using
spatially integrated quantities. We construct models with a range of constant
hydrogen densities between n$_H$ = 4 - 10 cm$^{-3}$ and a stellar wind-blown
cavity of 10 pc which reproduces the intensity and shape of most ionized gas
emission lines, including the high ionization lines [OIV] and [NeV], as well as
[SIII], [SIV], [OIII], and [NeIII]. Our models suggest that the majority of
[SiII] emission (91%) is produced at the edge of the HII region around the
transition between ionized and atomic gas while very little of the [CII]
emission (<5%) is associated with the ionized gas. The physical conditions of
N76 are characterized by a hot HII region with a maximum electron temperature
of T$_e$ ~ 24,000 K, electron densities that range from n$_e$ ~ 4 to 12
cm$^{-3}$, and high ionization parameters of log(U) ~ -1.15 to -1.77. By
analyzing a low metallicty WR nebula with a single ionization source, this work
gives valuable insights on the impact WR stars have to the galaxy-integrated
ionized gas properties in nearby dwarf galaxies.
