Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...293..216p&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 293, June 1, 1985, p. 216-229. Research supported by the Space Telescope Sc
Astronomy and Astrophysics
Astrophysics
92
Interstellar Matter, Molecular Clouds, Rotating Disks, Star Formation, Angular Momentum, Protostars, Stellar Cores, Stellar Mass Accretion, Stellar Mass Ejection, Stellar Winds
Scientific paper
This paper presents a theory for star formation in rotating molecular disks in which accretion onto the protostellar core produces FUV radiation which heats the disk surfaces out to large radii. A hydromagnetic wind results in which heated gas is driven out along field lines which thread the disk and are aligned with the disk rotation axis. The centrifugally driven wind removes angular momentum from the disk at rates high enough to brake it down to protostellar specific values in 105yr. The wind drives an accretion rate through the disk at rates which are consistent with the accretion luminosity. This global analysis of star formation in a rotating, magnetized disk offers a unifying scheme for understanding both star formation and bipolar outflows. The disks in which massive stars form are predicted to be dense (108cm-3) and have rotation speeds of 4 km s-1, scales of order 5×1016cm, masses of order 102M_sun;, and axial ratios of 0.2.
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