  Theoretical models indicate that photoevaporative and magnetothermal winds
play a crucial role in the evolution and dispersal of protoplanetary disks and
affect the formation of planetary systems. However, it is still unclear what
wind-driving mechanism is dominant or if both are at work, perhaps at different
stages of disk evolution. Recent spatially resolved observations by Fang et al.
(2023) of the [OI] 6300 Angstrom spectral line, a common disk wind tracer, in
TW Hya revealed that about 80% of the emission is confined to the inner few au
of the disk. In this work, we show that state-of-the-art X-ray driven
photoevaporation models can reproduce the compact emission and the line profile
of the [OI] 6300 Angstrom line. Furthermore, we show that the models also
simultaneously reproduce the observed line luminosities and detailed spectral
profiles of both the [OI] 6300 Angstrom and the [NeII] 12.8 micron lines. While
MHD wind models can also reproduce the compact radial emission of the [OI] 6300
Angstrom line, they fail to match the observed spectral profile of the [OI]
6300 Angstrom line and underestimate the luminosity of the [NeII] 12.8 micron
line by a factor of three. We conclude that, while we cannot exclude the
presence of an MHD wind component, the bulk of the wind structure of TW Hya is
predominantly shaped by a photoevaporative flow.
