Mass loss from rapidly rotating magnetic protostars

Details Mass loss from rapidly rotating magnetic protostars Mass loss from rapidly rotating magnetic protostars

May 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...328l..19s&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 328, May 1, 1988, p. L19-L23. NSF-NASA-supported research.

Astronomy and Astrophysics

Astrophysics

191

Accretion Disks, Magnetic Stars, Molecular Clouds, Protostars, Stellar Mass Ejection, Stellar Rotation, Angular Momentum, Magnetohydrodynamic Flow, Stellar Winds

Scientific paper

The authors propose that bipolar outflows from young stellar objects originate from a protostar rotating at breakup at its equator because it is being spun up by an adjoining accretion disk. Mass outflow at an appreciable fraction of the infall rate from a surrounding molecular cloud core onto the star and disk can be driven centrifugally if the protostar has a sufficiently strong magnetic field. The expansion of the flow toward the rotational poles may provide a collimation mechanism for focusing an ordinary stellar wind into optical jets.

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