Forbidden Lines and Disk Winds

Low excitation optical forbidden lines are one of the defining characteristics of accreting T Tauri stars. These lines are predominantly blueshifted, indicating winds and disk occultation, with profiles that can be decomposed into kinematic components attributed to high velocity collimated jets (HVC) and lower velocity disk winds (LVC). Recently the LVC has been further decomposed into two further kinematic components, a broad one (BC) attributed to an inner disk wind and a narrow one (NC) attributed to a slower outer disk wind. Using high resolution spectra from Keck's HIRES and Magellan's MIKE spectrograph for a sample of 65 T Tauri stars, 48 of which also include [SII 4068] as well as [OI 6300 and [OI 5577], we make a detailed comparison of these various kinematic components both with each other and with additional system properties such as inclination, accretion luminosity, and disk structure. Two important new findings are establishing a connection between the properties of the HVC and the LVC that point to a physical link between them, and determining forbidden line ratios that demonstrate the LVC components arise under conditions of thermal excitation, allowing mass loss rat