  The origin of radio emission in different populations of radio-quiet quasars
is relatively unknown, but recent work has uncovered various drivers of
increased radio-detection fraction. In this work, we pull together three known
factors: optical colour ($g-i$), \CIV Distance (a proxy for $L/L_{Edd}$) and
whether or not the quasar contains broad absorption lines (BALQSOs) which
signify an outflow. We use SDSS DR14 spectra along with the LOFAR Two Metre Sky
Survey Data Release 2 and find that each of these properties have an
independent effect. BALQSOs are marginally more likely to be radio-detected
than non-BALQSOs at similar colours and $L/L_{Edd}$, moderate reddening
significantly increases the radio-detection fraction and the radio-detection
increases with $L/L_{Edd}$ above a threshold for all populations. We test a
widely used simple model for radio wind shock emission and calculate energetic
efficiencies that would be required to reproduce the observed radio properties.
We discuss interpretations of these results concerning radio-quiet quasars more
generally. We suggest that radio emission in BALQSOs is connected to a
different physical origin than the general quasar population since they show
different radio properties independent of colour and \CIV distance.
