  We re-evaluate the outer edge of orbital stability for possible exomoons
orbiting the radial velocity planet discovered in the HD 23079 system. In this
system, a solar-type star hosts a Jupiter-mass planet in a nearly circular
orbit in the outer stellar habitable zone. The outer stability limit of
exomoons is deduced using $N$-body and tidal migration simulations considering
a large range of initial conditions, encompassing both prograde and retrograde
orbits. In particular, we extend previous works by evaluating many values in
the satellite mean anomaly to identify and exclude regions of quasi-stability.
Future observations of this system can make use of our results through a scale
factor relative to the currently measured minimum mass. Using a constant time
lag tidal model (Hut 1981), we find that plausible tidal interactions within
the system are insufficient to induce significant outward migration toward the
theoretical stability limit. While current technologies are incapable of
detecting exomoons in this system, we comment on the detectability of putative
moons through Doppler monitoring within direct imaging observations in view of
future research capacities.
