Icy moons around the ice giant planets may contain subsurface oceans. Their oceans could be detected and characterized using measurements of magnetic fields induced by the host planet’s time-varying magnetospheric field. We explore the possibility of detecting and characterizing subsurface oceans among the five major moons of Uranus—with a particular focus on Ariel—using spacecraft magnetometry measurements. We find that the magnetic field at each moon is dominated by the synodic frequency with amplitudes ranging from ~4 nT at Oberon up to ~300 nT at Miranda. If these bodies contain oceans with sufficient thicknesses (>~6-100 km) and conductivities (>2 S m^-1), the induced surface fields should have amplitudes exceeding the typical ~1 nT sensitivity of spacecraft magnetometry investigations. Furthermore, the magnetic field at the moons spans periods ranging from 1 to 10³ h. This could enable long-term measurements to separately constrain ocean and ice thicknesses and ocean salinity.