  The precession of astrophysical jets produced by active-galactic nuclei is
likely related to the dynamics of the accretion disks surrounding the central
supermassive black holes (BHs) from which jets are launched. The two main
mechanisms that can drive jet precession arise from Lense-Thirring precession
and tidal torquing. These can explain direct and indirect observations of
precessing jets; however, such explanations often utilize crude approximations
of the disk evolution and observing jet precession can be challenging with
electromagnetic facilities. Simultaneously, the Laser Interferometer Space
Antenna (LISA) is expected to measure gravitational waves from the mergers of
massive binary BHs with high accuracy and probe their progenitor evolution. In
this paper, we connect the LISA detectability of binary BH mergers to the
possible jet precession during their progenitor evolution. We make use of a
semi-analytic model that self-consistently treats disk-driven BH alignment and
binary inspiral and includes the possibility of disk breaking. We find that
tidal torquing of the accretion disk provides a wide range of jet precession
timescales depending on the binary separation and the spin direction of the BH
from which the jet is launched. Efficient disk-driven BH alignment results in
shorter timescales of $\sim 1$ yr which are correlated with higher LISA
signal-to-noise ratios. Disk breaking results in the longest possible times of
$\sim 10^7$ yrs, suggesting a deep interplay between the disk critical
obliquity (i.e. where the disk breaks) and jet precession. Studies such as ours
will help to reveal the cosmic population of precessing jets that are
detectable with gravitational waves.
