We present the results of two studies investigating the abundance and physical state of
polycyclic aromatic hydrocarbons (PAHs) in the Small Magellanic Cloud (SMC). Observations
with ISO and Spitzer have shown that PAHs are deficient in low-metallicity galaxies. In
particular, galaxies with 12 + log(O/H) < 8 show mid-IR SEDs and spectra
consistent with low PAH abundance. The SMC provides a unique opportunity to map the PAH
emission in a low-metallicity (12 + log(O/H) ~ 8) galaxy at high spatial
resolution and sensitivity to learn about the PAH life cycle. Using mid- and far-IR
photometry from the Spitzer Survey of the SMC (S3MC) and mid-IR spectral
mapping from the Spitzer Spectroscopic Survey of the SMC (S4MC) we determine
the PAH abundance across the galaxy. We find that the SMC PAH abundance is low compared to
the Milky Way and variable, with high abundance in molecular regions and low abundance in
the diffuse ISM. From the variations of the mid-IR band strengths, we show that PAHs in
the SMC are smaller and more neutral than their counterparts in more metal-rich galaxies.
Based on the results of these two studies we propose that PAHs in the SMC are formed with
a size distribution shifted towards smaller grains and are therefore easier to destroy
under typical diffuse ISM conditions. The distribution of PAH abundance in the SMC
suggests that PAH formation in molecular clouds is an important process. We discuss the
implications of these results for our understanding of the PAH life-cycle both at
low-metallicity and in the Milky Way.