  We investigate the physical structure and conditions of photodissociation
regions (PDRs) and molecular gas within the Pillars of Creation in the Eagle
Nebula using SOFIA FEEDBACK observations of the [C II] 158 micron line. These
observations are velocity resolved to 0.5 km s$^{-1}$ and are analyzed
alongside a collection of complimentary data with similar spatial and spectral
resolution: the [O I] 63 micron line, also observed with SOFIA, and rotational
lines of CO, HCN, HCO$^{+}$, CS, and N$_2$H$^{+}$. Using the superb spectral
resolution of SOFIA, APEX, CARMA, and BIMA, we reveal the relationships between
the warm PDR and cool molecular gas layers in context of the Pillars' kinematic
structure. We assemble a geometric picture of the Pillars and their
surroundings informed by illumination patterns and kinematic relationships and
derive physical conditions in the PDRs associated with the Pillars. We estimate
an average molecular gas density $n_{{\rm H}_2} \sim 1.3 \times 10^5$ cm$^{-3}$
and an average atomic gas density $n_{\rm H} \sim 1.8 \times 10^4$ cm$^{-3}$
and infer that the ionized, atomic, and molecular phases are in pressure
equilibrium if the atomic gas is magnetically supported. We find pillar masses
of 103, 78, 103, and 18 solar masses for P1a, P1b, P2, and P3 respectively, and
evaporation times of $\sim$1-2 Myr. The dense clumps at the tops of the pillars
are currently supported by the magnetic field. Our analysis suggests that
ambipolar diffusion is rapid and these clumps are likely to collapse within
their photoevaporation timescales.
