Jet simulations extending radially self-similar MHD models
arXiv:astro-ph/0507634 · doi:10.1111/j.1365-2966.2005.09945.x
Abstract
We perform a numerical simulation of magnetohydrodynamic radially self-similar jets, whose prototype is the Blandford & Payne analytical example. The reached final steady state is valid close to the rotation axis and also at large distances above the disk where the classical analytical model fails to provide physically acceptable solutions. The outflow starts with a sub-slow magnetosonic speed which subsequently crosses all relevant MHD critical points and corresponding magnetosonic separatrix surfaces. The characteristics are plotted together with the Mach cones and the super-fast magnetosonic outflow satisfies MHD causality. The final solution remains close enough to the analytical one which is thus shown to be topologically stable and robust for various boundary conditions.
11 pages, 8 figures, minor changes to match the version accepted by MNRAS
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- Stability and structure of analytical MHD jet formation models with a finite outer disk radius
- Numerical simulations of MHD jets from Keplerian accretion disks I-Recollimation shocks
- Resistive jet simulations extending radially self-similar magnetohydrodynamic models
- Velocity asymmetries in YSO jets: Intrinsic and extrinsic mechanisms
- 3D simulations of disc-winds extending radially self-similar MHD models
- Comparison of synthetic maps from truncated jet-formation models with YSO jet observations
- Large resistivity in numerical simulations of radially self-similar outflows
- Resistive MHD jet simulations with large resistivity
- Comparison of synthetic maps from truncated jet-formation models with YSO jet observations. II. The effect of varying inclinations