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Exomoon detections might be feasible with NASA's Kepler or ESA's upcomingPLATO mission or the ground-based E-ELT. To use observational resources mostefficiently we need to know where the largest, most easily detected moons canform. We explore the possibility of large exomoons by following the movement ofwater (H2O) ice lines in the accretion disks around young super-Jovian planets.We want to know how different heating sources in those disks affect the H2O icelines. We simulate 2D rotationally symmetric accretion disks in hydrostaticequilibrium around super-Jovian exoplanets. The energy terms in oursemi-analytical model -- (1) viscous heating, (2) planetary illumination, (3)accretional heating, and (4) stellar illumination -- are fed by precomputedplanet evolution tracks. We consider planets accreting 1 to 12 Jupiter massesat distances between 1 and 20 AU to a Sun-like star. Accretion disks aroundJupiter-mass planets closer than ~4.5 AU to Sun-like stars do not feature H2Oice lines, but the most massive super-Jovians can form icy satellites as closeas ~3 AU to Sun-like stars. Super-Jovian planets forming beyond ~5 AU can hostMars-mass moons. We study a broad range of disk parameters for planets at 5.2AU and find that the H2O ice lines are universally between ~15 and 30 Jupiterradii when the last generation of moons is forming. If the abundant populationof super-Jovian planets at ~1 AU formed in situ, then they should lack gianticy moons because their disks did not host H2O ice in the final stages ofaccretion. In the more likely case that these planets migrated to their currentlocations from beyond a few AU, they might be orbited by large, H2O-rich moons.In this case, Mars-mass ocean moons might be common in the stellar habitablezones. Future exomoon searches can provide powerful constraints on theformation and migration history of giant exoplanets.

Conditions for water ice lines and Mars-mass exomoons around accreting super-Jovian planets at 1 - 20 AU from Sun-like stars