  The phenomenon of changing-look (CL) behavior in active galactic nuclei (AGN)
is characterized by dramatic changes in luminosity and/or emission line
profiles over relatively short periods, ranging from months to years. The
origin of CL-AGNs remains a mystery, but one proposed explanation involves the
response of the inner AGN disk to tidal disruption events (TDEs) around the
supermassive black hole (SMBH). In this Letter, we calculate the predicted
frequency of AGN TDEs as a function of SMBH mass and compare the results to the
observed CL-AGN distribution. We find that if the fraction of CL-AGNs caused by
AGN-TDEs is high, then: (1) most SMBHs in CL-AGN are near maximal spin, with
the dimensionless spin parameter $a>0.9$; (2) AGN inner disks have a high
surface density ($\geq 10^{7}\, {\rm g\, cm^{-2}}$); (3) typical AGN lifetimes
are $\sim 10$-$100$ Myr; and (4) a nuclear star cluster initial mass function
(IMF) that scales as $\sim m_*^{-1.6}$ is preferred. Future observations of
CL-AGN will help constrain the fraction of CL-AGNs caused by AGN-TDEs, SMBH
spins, AGN lifetimes, and the nuclear star cluster IMF.
