CASSINELLI, JP; CONTI, PS; CASSINELLI, JP; SREENIVASAN, SR; KOENIGSBERGER, G; MONTMERLE, T; ... LOZINSKAYA, TA; + view all CASSINELLI, JP; CONTI, PS; CASSINELLI, JP; SREENIVASAN, SR; KOENIGSBERGER, G; MONTMERLE, T; WALBORN, NR; HAMANN, WR; BARLOW, MJ; LOZINSKAYA, TA; - view fewer (1991) WOLF-RAYET STELLAR WIND THEORY. IAU SYMP (143) 289 - 307.
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Two possible solutions to the Wolf-Rayet wind momentum problem are discussed: purely radiation driven wind theory, with multi-line effects, and Luminous Magnetic Rotator theory. Several recently developed radiative processes for enhancing M or v infinity are described, and it is concluded that only the winds of rather hot luminous Wolf-Rayet stars could possibly be driven by radiation. These stars should show evidence of acceleration at large radial distances. For the rapid rotators, it is possible to drive a dense equatorial outflow. Limits are discussed regarding the needed surface magnetic fields. With this model, the wind momentum problem is solved in a piece-wise fashion by having the large radio flux of Wolf-Rayet stars come from the equatorial zone and the broad P Cygni lines, arising in the polar wind. The Luminous Magnetic Rotator model can also be tested through observation, primarily through spectropolarimetry.
|Title:||WOLF-RAYET STELLAR WIND THEORY|
|Keywords:||RADIATION-DRIVEN WINDS, HOT LUMINOUS STARS, MASS-LOSS, MODEL, ENERGY|
|UCL classification:||UCL > School of BEAMS > Faculty of Maths and Physical Sciences > Physics and Astronomy|
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