  We present a survey of optical [OI] emission at 6300 \AA\ toward 65 TTauri
stars at the spectral resolution of $\sim7$ km/s. Past work identified a highly
blueshifted velocity component (HVC) tracing microjets, and a less blueshifted
low-velocity-component (LVC) attributed to winds. We focus here on the LVC
kinematics to investigate links between winds, jets, accretion, and disk
dispersal. We track the behavior of four types of LVC components: a broad and
narrow component ("BC" and "NC") in LVCs that are decomposed into two
Gaussians, which typically have an HVC, and the single-Gaussian LVC profiles
separated into those that have an HVC ("SCJ") and those that do not ("SC"). LVC
centroid velocities and line widths correlate with HVC equivalent width and
accretion luminosity, suggesting that LVC/winds and HVC/jets are kinematically
linked and connected to accretion. The deprojected HVC velocity correlates with
accretion luminosity, showing that faster jets come with higher accretion. BC
and NC kinematics correlate and their blueshifts are maximum at $\sim
35^{\circ}$, suggesting a conical wind geometry with this semi-opening angle.
Only SCs include $n_{13-31}$ up to $\sim3$ and their properties correlate with
this infrared index, showing that [OI] emission recedes to larger radii as the
inner dust is depleted, tracing less dense/hot gas and a decrease in wind
velocity. All together, these findings support a scenario where optically
thick, accreting inner disks launch radially-extended MHD disk winds that feed
jets, and where inner disk winds recede to larger radii and jets disappear in
concert with dust depletion.
