Left: Swift/XRT and UVOT/UVW1 lightcurves of TDE AT 2018fyk. The vertical colored lines denote transitions as traced by the alpha_ox parameter, shown in the right panel as a function of the bolometric Eddington fraction. Alpha_ox is equivalent to hardness for stellar-mass blackholes. We divide the evolution into 5 phases depending on the lightcurve and X-ray spectral behaviour. Alpha_ox is unconstrained in the quiescent state (E) due to the Swift/XRT upper limits, but is expected to soften (move to upper left corner) if it behaves similar to X-ray binaries. A new XMM-Newton exposure can confirm whether TDE AT2018fyk is behaving as a scaled-up X-ray binary . A typical error bar is shown in the top left corner of the right panel. The uncertainty in bolometric Eddington fraction is dominated by the intrinsic scatter in the M-sigma relation.