Magnetic collimation of protostellar winds into bipolar outflows

Details Magnetic collimation of protostellar winds into bipolar outflows Magnetic collimation of protostellar winds into bipolar outflows

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990nascp3084..232n&link_type=abstract

In NASA, Ames Research Center, The Interstellar Medium in External Galaxies: Summaries of Contributed Papers p 232-234 (SEE N91-

Computer Science

Bipolarity, Collimation, Luminosity, Magnetic Fields, Magnetohydrodynamics, Molecular Clouds, Star Formation, Stellar Winds, Algorithms, Computer Programs, Field Strength, Simulation, Thermal Energy

Scientific paper

Researchers describe self-consistent 2-D magnetohydrodynamic (MHD) simulations of the collimation of an isotropic protostellar wind into bipolar outflows by magnetic stresses in the ambient medium. A variety of ambient field strengths, wind luminosities, and density profiles were studied. Collimation occurs when the energy of the magnetic field swept up by the expanding bubble approaches the bubble thermal energy. Measured axial and radial expansion rates are in good agreement with the analytical predictions of Konigl (1982).

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