Astronomy and Astrophysics – Astrophysics
Scientific paper
2008-06-20
Astronomy and Astrophysics
Astrophysics
Accepted for publication in MNRAS
Scientific paper
10.1111/j.1365-2966.2008.13623.x
Numerical simulations with self-similar initial and boundary conditions provide a link between theoretical and numerical investigations of jet dynamics. We perform axisymmetric resistive magnetohydrodynamic (MHD) simulations for a generalised solution of the Blandford & Payne type, and compare them with the corresponding analytical and numerical ideal-MHD solutions. We disentangle the effects of the numerical and physical diffusivity. The latter could occur in outflows above an accretion disk, being transferred from the underlying disk into the disk corona by MHD turbulence (anomalous turbulent diffusivity), or as a result of ambipolar diffusion in partially ionized flows. We conclude that while the classical magnetic Reynolds number $R_{\rm m}$ measures the importance of resistive effects in the induction equation, a new introduced number, $\rbeta=(\beta/2)R_{\rm m}$ with $\beta$ the plasma beta, measures the importance of the resistive effects in the energy equation. Thus, in magnetised jets with $\beta<2$, when $\rbeta \la 1$ resistive effects are non-negligible and affect mostly the energy equation. The presented simulations indeed show that for a range of magnetic diffusivities corresponding to $\rbeta \ga 1$ the flow remains close to the ideal-MHD self-similar solution.
Cemeljic Miljenko
Gracia José
Tsinganos Kanaris
Vlahakis Nektarios
No associations
LandOfFree
Resistive jet simulations extending radially self-similar magnetohydrodynamic models does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Resistive jet simulations extending radially self-similar magnetohydrodynamic models, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Resistive jet simulations extending radially self-similar magnetohydrodynamic models will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-371570