Radiatively driven winds from magnetic, fast-rotating stars

Details Radiatively driven winds from magnetic, fast-rotating stars Radiatively driven winds from magnetic, fast-rotating stars

Jan 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986asee.nasa.....n&link_type=abstract

In NASA. Marshall Space Flight Center Research Reports: 1985 NASA/ASEE Summer Faculty Fellowship Program 16 p (SEE N86-24507

Statistics

Computation

Hot Stars, Magnetohydrodynamics, Stellar Magnetic Fields, Stellar Rotation, Stellar Winds, Acceleration (Physics), Computation, Mathematical Models, Momentum, Problem Solving, Thomson Scattering, Velocity Measurement

Scientific paper

An analytical procedure is developed to solve the magnetohydrodynamic equations for the stellar wind problem 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 treated relatively easily. Once the velocities at the critical points and the distances to the points are known, the streamline constants are determined in a straight-forward manner. This allows the structure of the wind to be elucidated without recourse to complicated computational schemes.

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