  We use Cloudy to re-examine excitation of [Oi] 6300 A and [Oi] 5577 A in the
X-ray driven photo-evaporative wind models of Owen and collaborators, and in
more recent magnetothermal models by Wang et al. We find that, at the measured
accretion luminosities, the FUV radiation would populate the upper levels of
the oxygen atom which would eventually contribute to the [Oi] lines. FUV
pumping competes with collisions as an excitation mechanism of the [Oi] lines,
and they each originate from a distinct region in the protostellar disk
environment depending on the specifics of the hydrodynamical model that the
simulation was based on. Consequently, the line strengths and shapes of [Oi]
6300 A and[Oi] 5577 A would be affected by the inclusion of FUV pumping in the
radiation transport simulations.

Solar and Stellar Astrophysics;Astrophysics of Galaxies