  This work provides evidence that a large fraction of \ion{C}{IV} narrow
absorption lines (NALs) seen along the line of sight to distant quasars are due
to accretion disk winds, while also seeking to understand the relationship
between NALs and certain quasar-intrinsic properties. We extend the results
from past work in the literature using $\sim105,000$ NALs from a sample of
$\sim58,000$ SDSS quasars. The primary results of this work are summarized as
follows: (1) the velocity distribution (${\rm d}N/{\rm d}\beta$) of NALs is not
a function of radio loudness (or even detection) once marginalized by
optical/UV luminosity; (2) there are significant differences in the number and
distribution of NALs as a function of both radio spectral index and optical/UV
luminosity, and these two findings are not entirely interdependent; (3)
improvements in quasar systemic redshift measurements and differences in the
NAL distribution as a combined function of optical luminosity and radio
spectral index together provide evidence that a significant portion of NALs are
due to outflows; (4) the results are consistent with standard models of
accretion disk winds governed by the $L_{\rm UV}$-$\alpha_{ox}$ relationship
and line-of-sight orientation indicated by radio spectral index, and (5)
possibly support a magnetically arrested disk model as an explanation for the
semi-stochastic nature of strong radio emission in a fraction of quasars.

Astrophysics of Galaxies