  For the majority of the tidal disruption event (TDE) candidates, the observed
energy in the optical/near-UV bands is of order 10^{51} erg. We show that this
observed energy is smaller than the minimum bolometric energy for the radiative
inefficient accretion flow model by a factor of 10-100. We argue that this
discrepancy is because the majority of the energy released is in the extreme-UV
(EUV) band and/or in the form of relativistic jets beamed away from the Earth.
The EUV scenario is supported by existing mid-infrared data and should be
further tested by future dust reverberation observations. The jet scenario is
disfavored by the radio observations of ASASSN-14li but may still be viable for
other TDE candidates. We also provide evidence that, at least for some TDEs,
most of the missing energy (in the EUV and/or in the form of jets) is released
within a few times the orbital period of the most tightly bound material, which
means (1) the circularization of the fallback stream may occur rapidly, and (2)
the luminosity of the accretion flow or the jet power may not be capped near
the Eddington level when the fallback rate is super-Eddington. For most other
TDEs, this energy-release timescale is currently not strongly constrained.
