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skydivephil
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How long does the bipolar outflow stage last in proto/T Tauri stars ?
A bipolar outflow in protostars is a phenomenon in which gas and dust are ejected from the poles of a protostar at high speeds. This outflow is often observed in young, forming stars and is thought to play a crucial role in the process of star formation.
A bipolar outflow is created through the interaction of a protostar's strong magnetic field and the surrounding gas and dust. As material falls onto the protostar, the magnetic field channels the material along the poles, causing it to be ejected at high speeds.
Bipolar outflows are important because they help to regulate the growth of a protostar. By removing excess material from the protostar's surrounding disk, the outflow prevents the protostar from becoming too massive and potentially disrupting the formation of planets around it.
Bipolar outflows in protostars are studied using a variety of methods, including radio, infrared, and optical observations. These observations allow scientists to measure the velocity and composition of the outflowing material, as well as the structure and dynamics of the surrounding gas and dust.
Yes, bipolar outflows are a common phenomenon in protostars. They have been observed in a wide range of star-forming regions and are thought to occur in the majority of protostars. However, the strength and duration of these outflows can vary greatly depending on the properties of the protostar and its surrounding environment.