Physics
Scientific paper
Oct 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978m%26p....19..261e&link_type=abstract
(Conference on Protostars and Planets, Tucson, Ariz., Jan. 3-7, 1978.) Moon and the Planets, vol. 19, Oct. 1978, p. 261-277.
Physics
43
Nebulae, Plasma Interactions, Stellar Mass Accretion, Stellar Winds, Angular Momentum, Disks (Shapes), Stellar Luminosity, Turbulence Effects
Scientific paper
The interaction between a strong stellar wind carrying no intrinsic angular momentum and a surrounding disk nebula is investigated. The shape and stability of the wind-nebula interface, the strength and direction of the ensuing mass motions, and the time scales for nebular disruption are analyzed. The dominant physical process is one of nebular accretion onto the central star due to turbulent viscosity in the disk. The turbulence will be driven in the upper layers of the disk by the wind. It is noted that if the accretion supplies mass for the wind (after the absorption of stellar energy), then the particle fluxes may undergo a runaway increase until the energy or momentum flux in the wind is limited by the total stellar luminosity. This may explain the origin of strong pre-main-sequence winds.
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