  In this work, we present a photospheric solar silicon abundance derived using
CO5BOLD model atmospheres and the LINFOR3D spectral synthesis code. Previous
works have differed in their choice of a spectral line sample and model
atmosphere as well as their treatment of observational material, and the solar
silicon abundance has undergone a downward revision in recent years. We
additionally show the effects of the chosen line sample, broadening due to
velocity fields, collisional broadening, model spatial resolution, and magnetic
fields. CO5BOLD model atmospheres for the Sun were used in conjunction with the
LINFOR3D spectral synthesis code to generate model spectra, which were then fit
to observations in the Hamburg solar atlas. We present a sample of 11 carefully
selected lines (from an initial choice of 39 lines) in the optical and
infrared, made possible with newly determined oscillator strengths for the
majority of these lines. Our final sample includes seven optical Si I lines,
three infrared Si I lines, and one optical Si II line. We derived a
photospheric solar silicon abundance of $\log \epsilon_\mathrm{Si} = 7.57 \pm
0.04$, including a $-0.01$ dex correction from Non-Local Thermodynamic
Equilibrium (NLTE) effects. Combining this with meteoritic abundances and
previously determined photospheric abundances results in a metal mass fraction
Z/X = $0.0220 \pm 0.0020$. We found a tendency of obtaining overly broad
synthetic lines. We mitigated the impact of this by devising a de-broadening
procedure. The over-broadening of synthetic lines does not substantially affect
the abundance determined in the end. It is primarily the line selection that
affects the final fitted abundance.
