  Properties of the Sun's interior can be determined accurately from
helioseismological measurements of solar oscillations. These measurements,
however, are in conflict with photospheric elemental abundances derived using
3-D hydrodynamic models of the solar atmosphere. This divergence of theory and
helioseismology is known as the $"$solar modeling problem$"$. One possible
solution is that the photospheric neon abundance, which is deduced indirectly
by combining the coronal Ne/O ratio with the photospheric O abundance, is
larger than generally accepted. There is some support for this idea from
observations of cool stars. The Ne/O abundance ratio has also been found to
vary with the solar cycle in the slowest solar wind streams and coronal
streamers, and the variation from solar maximum to minimum in streamers
($\sim$0.1 to 0.25) is large enough to potentially bring some of the solar
models into agreement with the seismic data. Here we use daily-sampled
observations from the EUV Variability Experiment (EVE) on the Solar Dynamics
Observatory taken in 2010--2014, to investigate whether the coronal Ne/O
abundance ratio shows a variation with the solar cycle when the Sun is viewed
as a star. We find only a weak dependence on, and moderate anti-correlation
with, the solar cycle with the ratio measured around 0.2--0.3 MK falling from
0.17 at solar minimum to 0.11 at solar maximum. The effect is amplified at
higher temperatures (0.3--0.6 MK) with a stronger anti-correlation and the
ratio falling from 0.16 at solar minimum to 0.08 at solar maximum. The values
we find at solar minimum are too low to solve the solar modeling problem.
