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Two dimensional time independent self-similar magnetohydrodynamic equations are used to model bipolar outflows from young stellar objects. In this analysis, no pre-existing structures such as accretion disks or dense toroidal gas clouds are assumed; this approach is global in nature and all such structures must emerge as natural consequences of the model. Global numerical solutions are constructed which extend from the equator to the poles. Preliminary solutions to the simplest models demonstrating plausible density variations and high axial outflow velocities near the star will be presented.
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