  The decades-long explorations on the dispersal of protoplanetary disks
involve many debates about photoevaporation versus magnetized wind launching
mechanisms. This letter argues that the observed winds originating from the
inner disk ($R\lesssim 0.3$ AU) cannot be explained by the photoevaporative
mechanism. Energy conservation requires the presumed photoevaporative winds to
be heated to $\gtrsim 10^5$ K when launched from inner disks. However, due to
efficient thermal accommodation with dust grains and cooling processes at high
densities, X-ray irradiation at energies above 1 keV cannot efficiently launch
winds in the first place because of its high penetration. Some studies claiming
X-ray wind launching have oversimplified the thermochemical couplings.
Furthermore, heating the gas to escape velocity will over-ionize it,
suppressing the species responsible for observed forbidden lines (e.g., [OI]
6300 $\r{A}$ ). Confirmed by semi-analytic integrations of thermochemical fluid
structures, such high ionizations contradict the observed emission of neutral
and singly-ionized atoms from the winds originating from the inner disks.
