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We analyze high-resolution (dv=<10km/s) optical and infrared spectra coveringthe [OI] 6300 angstrom and [NeII] 12.81 micron lines from a sample of 31 disksin different evolutionary stages. Following work at optical wavelengths, we useGaussian profiles to fit the [NeII] lines and classify them into HVC (LVC) ifthe line centroid is more (less) blueshifted than 30 km/s with respect to thestellar radial velocity. Unlike for the [OI] where a HVC is often accompaniedby 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 dustdisk depletes (higher n13-31) the [NeII] luminosity increases while the [OI]weakens. The [NeII] and [OI] HVC profiles are generally similar with centroidsand FWHMs showing the expected behaviour from shocked gas in micro-jets. Incontrast, the [NeII] LVC profiles are typically more blueshifted and narrowerthan the [OI] profiles. The FWHM and centroid vs. disk inclination suggest thatthe [NeII] LVC predominantly traces unbound gas from a slow, wide-angle windthat 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, mostlymolecular, MHD winds.

The Evolution of Disk Winds from a Combined Study of Optical and Infrared Forbidden Lines