  We analyze high-resolution (dv=<10km/s) optical and infrared spectra covering
the [OI] 6300 angstrom and [NeII] 12.81 micron lines from a sample of 31 disks
in different evolutionary stages. Following work at optical wavelengths, we use
Gaussian profiles to fit the [NeII] lines and classify them into HVC (LVC) if
the line centroid is more (less) blueshifted than 30 km/s with respect to the
stellar radial velocity. Unlike for the [OI] where a HVC is often accompanied
by a LVC, all 17 sources with a [NeII] detection have either a HVC or a LVC.
[NeII] HVCs are preferentially detected toward high accretors (Macc > 10$^{-8}$
Msun/yr) while LVCs are found in sources with low Macc, low [OI] luminosity,
and large infrared spectral index (n13-31). Interestingly, the [NeII] and [OI]
LVC luminosities display an opposite behaviour with n13-31: as the inner dust
disk depletes (higher n13-31) the [NeII] luminosity increases while the [OI]
weakens. The [NeII] and [OI] HVC profiles are generally similar with centroids
and FWHMs showing the expected behaviour from shocked gas in micro-jets. In
contrast, the [NeII] LVC profiles are typically more blueshifted and narrower
than the [OI] profiles. The FWHM and centroid vs. disk inclination suggest that
the [NeII] LVC predominantly traces unbound gas from a slow, wide-angle wind
that has not lost completely the Keplerian signature from its launching region.
We sketch an evolutionary scenario that could explain the combined [OI] and
[NeII] results and includes screening of hard (~1keV) X-rays in inner, mostly
molecular, MHD winds.
