  Monte Carlo calculations of the Ne K$\alpha$ line fluoresced by coronal
x-rays and emitted near the temperature minimum region of the solar atmosphere
have been employed to investigate the use of this feature to measure directly
the solar photospheric Ne abundance. Though very weak, comparison with spectral
line databases indicates that at plasma temperatures typical of the quiet Sun
and cool active regions ($\leq 2\times 10^6$ K) the line is isolated and
unblended. A canonical solar chemical composition yields an equivalent width of
$\sim 6$ m\AA (0.3 eV) when observed at heliocentric angles $\sim 0$. For a 1
arcmin field of view, photon fluxes at Earth are of order 0.2 ph s$^{-1}$ for
the quiet Sun, rendering the Ne K$\alpha$ fluorescent line a quite feasible
means for determining the solar photospheric Ne content.
