model-e bâd-e X
Fr.: modèle de vent X
A → magnetocentrifugal model for → accretion and → outflow in → protostars, which considers the interaction between the → magnetosphere of a → young stellar object and an & rarr; accretion disk. The model assumes that the → magnetic field originates from the protostar, and the outflow is driven from a small region near the inner edge of the disk, called X, where the inner disk corotates with the star (→ corotation radius). The accretion disk is → truncated in its central region, that is the disk does not extend to the protostar. The matter spiraling toward the protostar is either funneled by the magnetic field connecting the star to the disk, or blown outward under the effect of → centrifugal force. The X-wind model is able to account for many observations in one fairly self-consistent model. The observations include time variable accretion/wind phenomena in → T Tauri stars, the slow rotation rates of T Tauri stars, protostellar X-ray activity, and a number of the properties of → bipolar jets and → molecular outflows (F. H. Shu et al., 2000, in Protostars and Planets IV, V. Mannings et al. (eds.), Tucson: Univ. Arizona Press, 789).