The structure of protostellar accretion disks and the origin of bipolar flows

Details The structure of protostellar accretion disks and the origin of bipolar flows The structure of protostellar accretion disks and the origin of bipolar flows

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...410..218w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 410, no. 1, p. 218-238.

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182

Accretion Disks, Molecular Flow, Protostars, Stellar Magnetic Fields, Astronomical Models, Computational Astrophysics, Differential Equations, Magnetohydrodynamics

Scientific paper

Equations are obtained which govern the disk-wind structure and identify the physical parameters relevant to circumstellar disks. The system of equations is analyzed in the thin-disk approximation, and it is shown that the system can be consistently reduced to a set of ordinary differential equations in z. Representative solutions are presented, and it is shown that the apparent paradox discussed by Shu (1991) is resolved when the finite thickness of the disk is taken into account. Implications of the results for the origin of bipolar flows in young stellar objects and possible application to active galactic nuclei are discussed.

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