Issue |
A&A
Volume 428, Number 2, December III 2004
|
|
---|---|---|
Page(s) | 545 - 554 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20040325 | |
Published online | 26 November 2004 |
The influence of rotation in radiation driven winds from hot stars
II. CAK topological analysis
1
Departamento de Física y Meteorología, Facultad de Ciencias, Universidad de Valparaíso, Valparaíso, Chile e-mail: michel.cure@uv.cl
2
Departamento de Matemáticas, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, Argentina e-mail: drial@dm.uba.ar
Received:
24
February
2004
Accepted:
26
August
2004
The topological analysis from Bjorkman ([CITE]) for the standard model that describes the winds from hot stars by Castor et al. ([CITE]) has been extended to include the effect of stellar rotation and changes in the ionization of the wind.
The differential equation for the momentum of the wind is non-linear and transcendental for the velocity gradient. Due to this non-linearity the number of solutions that this equation possess is not known. After a change of variables and the introduction of a new physically meaningless independent variable, we manage to replace the non-linear momentum differential equation by a system of differential equations where all the derivatives are explicitely given. We then use this system of equations to study the topology of the rotating-CAK model. For the particular case when the wind is frozen in ionization () only one physical solution is found, the standard CAK solution, with a X-type singular point. For the more general case (
), besides the standard CAK singular point, we find a second singular point which is focal-type (or attractor). We find also, that the wind does not adopt the maximal mass-loss rate but almost the minimal.
Key words: hydrodynamics / methods: analytical / stars: early-type / stars: mass-loss / stars: rotation / stars: winds, outflows
© ESO, 2004
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