The following conclusions about the kinematics and parameters of the gas in the vicinity of TW Hya have been drawn from an analysis of optical and ultraviolet line profiles and intensities. The accreting matter rises in the magnetosphere to a distance z>R* above the disk plane and falls to the star near its equator almost perpendicular to its plane. The matter outflows from a disk region with an outer radius of < 0.5 AU. The [OI], [SII], and H2 lines originate in the disk atmosphere outside the outflow region, where the turbulent gas velocity is close to the local speed of sound. In the formation region of the forbidden lines, T ~ 8500 K and Ne ~ 5 x 106 cm-3, and the hydrogen is almost neutral: xe < 0.03. The absorption features observed in the blue wings of some of the ultraviolet lines originate in the part of the wind that moves almost perpendicular to the disk plane, i.e., in the jet of TW Hya. The Vz gas velocity component in the jet decreases with increasing distance from the jet axis from 200 to 30 km/s. The matter outflowing from the inner disk boundary, moves perpendicular to the disk plane in the formation region of blue absorption line components, at a distance of ~0.5 AU from the axis of symmetry of the disk. This region of the wind is collimated into the jet at a distance of < 3 AU from the disk plane. The gas temperature in the formation region of absorption components is ~ 2 x 104 K, and the gas density is < 3 x 106 cm-3. This region of the jet is on the order of several AU away from the disk plane, while free recombination in the jet begins even farther from the disk. The mass-loss rate for TW Hya is M-dotw < 7 x 10-10 Msolar yr-1, which is a factor of 3 lower than the mean accretion rate. The relative abundance of silicon and aluminum in the jet gas is at least an order of magnitude lower than its standard value.