  Understanding how the solar corona is structured is of fundamental importance
to determining how the Sun's upper atmosphere is heated to high temperatures.
Recent spectroscopic studies have suggested that an instrument with a spatial
resolution of 200km or better is necessary to resolve coronal loops. The High
Resolution Coronal Imager (Hi-C) achieved this performance on a rocket flight
in July 2012. We use Hi-C data to measure the Gaussian widths of 91 loops
observed in the solar corona and find a distribution that peaks at about 270km.
We also use Atmospheric Imaging Assembly (AIA) data for a subset of these loops
and find temperature distributions that are generally very narrow. These
observations provide further evidence that loops in the solar corona are often
structured at a scale of several hundred kilometers, well above the spatial
scale of many proposed physical mechanisms.
