Radiatively driven winds from magnetic, fast-rotating stars - Wolf-Rayet stars?

Details Radiatively driven winds from magnetic, fast-rotating stars - Wolf-Rayet stars? Radiatively driven winds from magnetic, fast-rotating stars - Wolf-Rayet stars?

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...321..355n&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 321, Oct. 1, 1987, p. 355-369. NASA-supported research.

Statistics

Computation

14

Hot Stars, Magnetic Stars, Stellar Rotation, Stellar Winds, Wind Velocity, Wolf-Rayet Stars, Computational Astrophysics, Magnetohydrodynamic Flow, Optical Thickness, Plasma-Electromagnetic Interaction, Stellar Mass Ejection

Scientific paper

An analytical procedure is developed to solve the MHD equations for a stellar wind in the strong-magnetic-field, optically thick limit for hot stars. The slow-mode, Alfven, and fast-mode critical points are modified by the radiation terms in the force equation but in a manner that can be easily treated. Once the velocities and distances are known at the critical points, the streamline constants are determined in a straight-forward manner. This shows the structure of the wind with a relatively simple numerical scheme. The magnetic field and a radiation parameter specify the terminal wind velocity. High rotation rates and a modified slow-mode critical point close to the stellar surface determine the high mass-loss rates. Wolf-Rayet stars are modeled with 1000-G fields but require stellar rotational velocities approaching breakup values. The physical conditions that correspond to Wolf-Rayet models are so rare that another mechanism must be operating in these winds.

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