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We present the first remote sensing observations of the impact from a CoronalMass Ejection (CME) on the thermodynamic properties of the solar corona between1 and 3 Rs. Measurements of the Fe XI (789.2 nm) and Fe XIV (530.3 nm) emissionwere acquired with identical narrow-bandpass imagers at three observing sitesduring the 2017 August 21 Total Solar Eclipse. Additional continuum imagerswere used to observe K+F corona scattering, which is critical for thediagnostics presented here. The total distance between sites along the path oftotality was 1400 km, corresponding to a difference of 28 minutes between thetimes of totality at the first and last site. These observations were used tomeasure the Fe XI and Fe XIV emission relative to continuum scattering, as wellas the relative abundance of Fe 10+ and Fe 13+ from the line ratio. Theelectron temperature (Te) was then computed via theoretical ionizationabundance values. We find that the range of Te is 1.1-1.2 x10^6 K in coronalholes and 1.2-1.4 x10^6 K in streamers. Statistically significant changes of Teoccurred throughout much of the corona between the sites as a result ofserendipitous CME activity prior to the eclipse. These results underscore theunique advantage of multi-site and multi-wavelength total solar eclipseobservations for probing the dynamic and thermodynamic properties of the coronaover an uninterrupted distance range from 1 to 3 Rs.

astrophysical journal/the astrophysical journal

CME Induced Thermodynamic Changes in the Corona as Inferred from Fe XI  and Fe XIV Emission Observations during the 2017 August 21 Total Solar  Eclipse