  We present the first remote sensing observations of the impact from a Coronal
Mass Ejection (CME) on the thermodynamic properties of the solar corona between
1 and 3 Rs. Measurements of the Fe XI (789.2 nm) and Fe XIV (530.3 nm) emission
were acquired with identical narrow-bandpass imagers at three observing sites
during the 2017 August 21 Total Solar Eclipse. Additional continuum imagers
were used to observe K+F corona scattering, which is critical for the
diagnostics presented here. The total distance between sites along the path of
totality was 1400 km, corresponding to a difference of 28 minutes between the
times of totality at the first and last site. These observations were used to
measure the Fe XI and Fe XIV emission relative to continuum scattering, as well
as the relative abundance of Fe 10+ and Fe 13+ from the line ratio. The
electron temperature (Te) was then computed via theoretical ionization
abundance values. We find that the range of Te is 1.1-1.2 x10^6 K in coronal
holes and 1.2-1.4 x10^6 K in streamers. Statistically significant changes of Te
occurred throughout much of the corona between the sites as a result of
serendipitous CME activity prior to the eclipse. These results underscore the
unique advantage of multi-site and multi-wavelength total solar eclipse
observations for probing the dynamic and thermodynamic properties of the corona
over an uninterrupted distance range from 1 to 3 Rs.
