  Total solar eclipses (TSEs) provide a unique opportunity to quantify the
properties of the K-corona (electrons), F-corona (dust) and E-corona (ions)
continuously from the solar surface out to a few solar radii. We apply a novel
inversion method to separate emission from the K- and F-corona continua using
unpolarized total brightness (tB) observations from five 0.5 nm bandpasses
acquired during the 2019 July 2 TSE between 529.5 nm and 788.4 nm. The
wavelength dependence relative to the photosphere (i.e., color) of the F-corona
itself is used to infer the tB of the K- and F-corona for each line-of-sight.
We compare our K-corona emission results with the Mauna Loa Solar Observatory
(MLSO) K-Cor polarized brightness (pB) observations from the day of the
eclipse, and the forward modeled K-corona intensity from the Predictive Science
Inc. (PSI) Magnetohydrodynamic (MHD) model prediction. Our results are
generally consistent with previous work and match both the MLSO data and
PSI-MHD predictions quite well, supporting the validity of our approach and of
the PSI-MHD model. However, we find that the tB of the F-corona is higher than
expected in the low corona, perhaps indicating that the F-corona is slightly
polarized -- challenging the common assumption that the F-corona is entirely
unpolarized.

Solar and Stellar Astrophysics