## Outflows from magnetic rotators## I. Inner structure
^{1} Observatoire de Strasbourg 11 rue de l'Université
F-67000 Strasbourg, France^{2} Department of Physics, Queen's University, Kingston,
Ontario, K7L 3N6, Canada^{3} Institut für Angewandte Mathematik, Universität
Heidelberg, Im Neuenheimer Feld 293, D-69120 Heidelberg, Germany^{4} Space Telescope Science Institute and Johns Hopkins
University, 3700 San Martin Drive, Baltimore, MD 21218, USA
A simplified model for the stationary, axisymmetric structure of
magnetized winds with a polytropic equation of state is presented. The
shape of the magnetic surfaces is assumed to be known (conical in this
paper) within the fast magnetosonic surface. The model is
non-self-similar. Rather than solving the equilibrium perpendicular to
the flux surfaces everywhere, solutions are found at the Alfvèn
surface where it takes the form of the Alfvèn regularity
condition and at the base of the flow. This constrains the Transfield
equilibrium in that the Alfvèn regularity condition is imposed
and the regularity of the magnetic surfaces at the Alfvèn
critical surface is ensured. The model imposes criticality conditions
at the slow and fast magnetosonic critical points using the Bernoulli
equation. These Alfvén regularity and criticality conditions
are used to evaluate three constants of motion, the total energy,
angular momentum, and the ratio of mass to magnetic flux
, as well as the shape of the critical surfaces.
The rotation rate and the polytropic constant
This article contains no SIMBAD objects. ## Contents- 1. Introduction
- 2. Properties of MHD winds
- 2.1. A model for the structure of rotating MHD winds
- 2.2. Analytical method
- 2.2.1. General procedure
- 2.2.2. A general constraint
- 2.3. Numerical method
- 3. The solar wind
- 4. Jets from YSOs
- 4.1. Stellar winds ()
- 4.1.1. Fast cold rotator
- 4.1.2. An example of TTauri star: BP Tau
- 4.1.3. Effects of the amplitude of the mass loss
- 4.1.4. Rotational effects
- 4.1.5. Thermal effects
- 4.1.6. Limit cases
- 4.1.7. Discussion
- 4.2. Other variations of and
*Q*- 4.2.1. Non-constant
- 4.2.2. Non-constant
*Q*
- 4.1. Stellar winds ()
- 5. Intermediate rotator
- 6. Discussions
- 7. Conclusions
- Appendix
- References
© European Southern Observatory (ESO) 1998 Online publication: August 17, 1998 |