  The dust emissivity spectral index, $\beta$, is a critical parameter for
deriving the mass and temperature of star-forming structures, and consequently
their gravitational stability. The $\beta$ value is dependent on various dust
grain properties, such as size, porosity, and surface composition, and is
expected to vary as dust grains evolve. Here we present $\beta$, dust
temperature, and optical depth maps of the star-forming clumps in the Perseus
Molecular Cloud determined from fitting SEDs to combined Herschel and JCMT
observations in the 160 $\mu$m, 250 $\mu$m, 350 $\mu$m, 500 $\mu$m, and 850
$\mu$m bands. Most of the derived $\beta$, and dust temperature values fall
within the ranges of 1.0 - 2.7 and 8 - 20 K, respectively. In Perseus, we find
the $\beta$ distribution differs significantly from clump to clump, indicative
of grain growth. Furthermore, we also see significant, localized $\beta$
variations within individual clumps and find low $\beta$ regions correlate with
local temperature peaks, hinting at the possible origins of low $\beta$ grains.
Throughout Perseus, we also see indications of heating from B stars and
embedded protostars, as well evidence of outflows shaping the local landscape.
