  We explore the accretion states of tidal disruption events (TDEs) using a
sample of 7 X- ray bright sources. To this end, we estimate the relative
contribution of the disk and corona to the observed X-ray emission through
spectral modeling, and assess the X-ray brightness (through ${\alpha}$_ox,
L$_{2 keV}$ and f$_{Edd,X}$) as a function of the Eddington ratio. We report
strong positive correlations between ${\alpha}$_ox and f$_{Edd,bol}$;
f$_{Edd,X}$ and f$_{Edd,UV}$ ; and an anti-correlation for L$_{2 keV}$ and
f$_{Edd,UV}$. TDEs at high f$_{Edd,bol}$ have thermal dominated X-ray spectra
and high (soft) ${\alpha}$_ox, whereas those at low f$_{Edd,bol}$ show a
significant power-law contribution and low (hard) ${\alpha}$_ox. Similar to
X-ray binaries and active galactic nuclei, the transition between X-ray
spectral states occurs around f$_{Edd,bol}$ ${\approx}$ 0.03, although the
uncertainty is large due to the small sample size. Our results suggest that
X-ray surveys are more likely to discover TDEs at low f$_{Edd,bol}$, whereas
optical surveys are more sensitive to TDEs at high Eddington ratios. The X-ray
and optical selected TDEs have different UV and X-ray properties, which should
be taken into account when deriving rates, luminosity and black hole mass
functions. TDEs around the most massive supermassive black holes are observed
in the hard state; this could indicate that TDE evolution is faster around more
massive BHs.
