Pascucci, IlariaIlariaPascucciBanzatti, AndreaAndreaBanzattiGorti, UmaUmaGortiFang, MinMinFangPontoppidan, KlausKlausPontoppidanAlexander, RichardRichardAlexanderBallabio, GiuliaGiuliaBallabioEdwards, SuzanSuzanEdwardsSalyk, ColetteColetteSalykSACCO, GIUSEPPE GERMANOGIUSEPPE GERMANOSACCOFLACCOMIO, EttoreEttoreFLACCOMIOBlake, Geoffrey A.Geoffrey A.BlakeCarmona, AndresAndresCarmonaHall, CassandraCassandraHallKamp, IngaIngaKampKäufl, Hans UlrichHans UlrichKäuflMeeus, GwendolynGwendolynMeeusMeyer, MichaelMichaelMeyerPauly, TylerTylerPaulySteendam, SimonSimonSteendamSterzik, MichaelMichaelSterzik2022-02-112022-02-1120200004-637Xhttp://hdl.handle.net/20.500.12386/31387We analyze high-resolution (Δv ≤ 10 km s<SUP>-1</SUP>) optical and infrared spectra covering the [O I] λ6300 and [Ne II] 12.81 μm lines from a sample of 31 disks in different evolutionary stages. Following work at optical wavelengths, we use Gaussian profiles to fit the [Ne II] lines and classify them into high-velocity component (HVC) or low-velocity component (LVC) if the line centroid is more or less blueshifted than 30 km s<SUP>-1</SUP> with respect to the stellar radial velocity, respectively. Unlike for the [O I], where an HVC is often accompanied by an LVC, all 17 sources with an [Ne II] detection have either an HVC or an LVC. [Ne II] HVCs are preferentially detected toward high accretors ( ${\dot{M}}_{\mathrm{acc}}\gt {10}^{-8}$ M<SUB>⊙</SUB> yr<SUP>-1</SUP>), while LVCs are found in sources with low ${\dot{M}}_{\mathrm{acc}}$ , low [O I] luminosity, and large infrared spectral index (n<SUB>13-31</SUB>). Interestingly, the [Ne II] and [O I] LVC luminosities display an opposite behavior with n<SUB>13-31</SUB>: as the inner dust disk depletes (higher n<SUB>13-31</SUB>), the [Ne II] luminosity increases while the [O I] weakens. The [Ne II] and [O I] HVC profiles are generally similar, with centroids and FWHMs showing the expected behavior from shocked gas in microjets. In contrast, the [Ne II] LVC profiles are typically more blueshifted and narrower than the [O I] profiles. The FWHM and centroid versus disk inclination suggest that the [Ne II] 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 [O I] and [Ne II] results and includes screening of hard (∼1 keV) X-rays in inner, mostly molecular, MHD winds.STAMPAenArticle10.3847/1538-4357/abba3c2-s2.0-85096062506WOS:000585690100001https://api.elsevier.com/content/abstract/scopus_id/85096062506https://iopscience.iop.org/article/10.3847/1538-4357/abba3c2020ApJ...903...78PFIS/05 - ASTRONOMIA E ASTROFISICAERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation