Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986cajph..64..501p&link_type=abstract
(Conference on Jets from Stars and Galaxies, Toronto, Canada, June 24-27, 1985) Canadian Journal of Physics (ISSN 0008-4204), vo
Astronomy and Astrophysics
Astronomy
12
Accretion Disks, Magnetohydrodynamic Flow, Protostars, Star Formation, Stellar Winds, Angular Momentum, Cataclysmic Variables, Collimation, Ionized Gases, Molecular Gases, Radio Jets (Astronomy)
Scientific paper
A hydromagnetic wind model for molecular and ionized gas outflows associated with protostars is presented. If the luminosity of protostars is due to accretion, then centrifugally driven winds that arise from the envelopes of molecular disks explain the observed rates of momentum and energy transport. Ionized outflow originates from disk radii about 10 to the 15th cm or less, inside of which Ly-continuum photons from the protostellar accretion shock are intercepted. Observed molecular outflows arise from the cool disk envelope at radii between 10 to the 15th and 10 to the 17th cm. The mass-loss rates of these two component outflows are M(ion) about 10 to the -6th solar mass/yr and 10 to the -4th solar mass/yr, respectively. These winds solve the angular-momentum problem of star formation. It is proposed that the collimation of such outflows is due to 'hoop' stresses generated by the increasingly toroidal magnetic field in the wind and suggest that the structure of the underlying disks makes self-similar solutions for these outflows likely.
Norman Colin A.
Pudritz Ralph E.
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