  Giant, star-forming clumps are a common feature prevalent amongst
high-redshift star-forming galaxies and play a critical role in shaping their
chaotic morphologies and yet, their nature and role in galaxy evolution remains
to be fully understood. A majority of the effort to study clumps has been
focused at high redshifts, and local clump studies have often suffered from
small sample sizes. In this work, we present an analysis of clump properties in
the local universe, and for the first time, performed with a statistically
significant sample. With the help of the citizen science-powered Galaxy Zoo:
Hubble project, we select a sample of 92 $z<0.06$ clumpy galaxies in Sloan
Digital Sky Survey Stripe 82 galaxies. Within this sample, we identify 543
clumps using a contrast-based image analysis algorithm and perform photometry
as well as estimate their stellar population properties. The overall properties
of our $z<0.06$ clump sample are comparable to the high-redshift clumps.
However, contrary to the high-redshift studies, we find no evidence of a
gradient in clump ages or masses as a function of their galactocentric
distances. Our results challenge the inward migration scenario for clump
evolution for the local universe, potentially suggesting a larger contribution
of ex-situ clumps and/or longer clump migration timescales.
