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Magnetically driven jets and winds
Lovelace, R. V. E.; Berk, H. L.; Contopoulos, J.
AA(Texas, University, Austin), AB(Texas, University, Austin), AC(Cornell University, Ithaca, NY)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 379, Oct. 1, 1991, p. 696-705. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Computational Astrophysics, Jet Flow, Magnetohydrodynamic Flow, Protostars, Stellar Mass Accretion, Stellar Winds, Stellar Luminosity, Stellar Magnetic Fields, Stellar Rotation
Bibliographic Code:


Four equations for the origin and propagation of nonrelativistic jets and winds are derived from the basic conservation laws of ideal MHD. The axial current density is negative in the vicinity of the axis and positive at larger radii; there is no net current because this is energetically favored. The magnetic field is essential for the jet solutions in that the zz-component of the magnetic stress acts, in opposition to gravity, to drive matter through the slow magnetosonic critical point. For a representative self-consistent disk/jet solution relevant to a protostellar system, the reaction of the accreted mass expelled in the jets is 0.1, the ratio of the power carried by the jets to the disk luminosity is 0.66, and the ratio of the boundary layer to disk luminosities is less than about 0.13. The star's rotation rate decreases with time even for rotation rates much less than the breakup rate.

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