The arXiv preprint (v1 submitted May 2026) presents six years of simultaneous UV and X-ray monitoring of the nearby Seyfert galaxy ESO 511-G030, capturing a UV flux rise exceeding an order of magnitude in under three years. This single-object campaign, using XMM-Newton, Swift, and ground-based optical data, directly tracks the recovery of an optically thick accretion disk rather than a simple uncovering event. At rates above ~1% Eddington the disk-corona coupling follows the nonlinear relation seen in luminous quasars, but below this threshold the correlation breaks, consistent with inner-disk evaporation into a hot, optically thin flow. The study is a preprint and has not yet undergone peer review, limiting immediate generalizability. Prior monitoring campaigns on objects such as NGC 5548 (Peterson et al. 2002, ApJ) and the broader sample in Noda & Done (2018, MNRAS) hinted at similar state changes but lacked the dense, broadband cadence achieved here. The new data supply rare empirical anchors for simulations of truncated disks, confirming that radiatively efficient flows around supermassive black holes undergo transitions analogous to those in stellar-mass systems. Limitations include reliance on one source and potential aliasing of longer-term variability; future multi-year campaigns with XRISM and Athena will be needed to test universality.