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

Updated Studies on Exomoons in the HD 23079 System