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Simulating Magnetized Jets

  • Rony Keppens
  • Hubert Baty
  • Jeroen Bergmans
  • Fabien Casse

Abstract

A suitable model for the macroscopic behavior of accretion disk-jet systems is provided by the equations of MagnetoHydroDynamics (MHD). These equations allow us to perform scale-encompassing numerical simulations of multidimensional nonlinear magnetized plasma flows. For that purpose, we continue the development and exploitation of the Versatile Advection Code (VAC) along with its recent extension which employs dynamically controlled grid adaptation. In the adaptive mesh refinement AMRVAC code, modules for simulating any-dimensional special relativistic hydro- and magnetohydrodynamic problems are currently operational.

Here, we review recent 3D MHD simulations of fundamental plasma instabilities, relevant when dealing with cospatial shear flow and twisted magnetic fields. Such magnetized jet flows can be sus­ceptible to a wide variety of hydro (e.g. Kelvin—Helmholtz) or magnetohydrodynamic (e.g. current driven kink) instabilities. Recent MHD computations of 3D jet flows have revealed how such mutually interacting instabilities can in fact aid in maintaining jet coherency. Another breakthrough from com­putational magnetofluid modeling is the demonstration of continuous, collimated, transmagnetosonic jet launching from magnetized accretion disks.

Summarizing, MHD simulations are rapidly gaining realism and significantly advance our under­standing of nonlinear astrophysical magnetofluid dynamics.

Keywords

Jets MHD numerical 

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References

  1. Baty, H. and Keppens, R.: 2002, ApJ. 580, 800.ADSCrossRefGoogle Scholar
  2. Bergmans, J., Keppens, R., van Odyck, D.E.A. and Achterberg, A.: to appear in “Adaptive Mesh Refinement — Theory and Applications”, T. Plewa, T. Linde and V.G. Weirs (eds.), Spinger Lecture Notes in Computational Science and Engineering, 2004 (Proceedings of AMR2003, Chicago Workshop on Adaptive Mesh Refinement Methods, September 3–5, 2003, Chicago, USA )Google Scholar
  3. Casse, E. and Keppens, R.: 2002, ApJ 581, 988.ADSCrossRefGoogle Scholar
  4. Casse, E. and Keppens, R.: 2004, ApJ 601, 90.ADSCrossRefGoogle Scholar
  5. Ferreira, J.: 1996, in: W. Kundt (ed.), Jets from Stars and Galactic Nuclei, Proceedings Bad Honnef, Germany, 1995, p. 82.Google Scholar
  6. Keppens, R. and Tóth, G.: 1999, Phys. Plasmas 6, 1461.MathSciNetADSCrossRefGoogle Scholar
  7. Keppens, R., Nool, M., Tóth, G. and Goedbloed, J.P.: 2003, Comput. Physics Comm. 153, 317ADSMATHCrossRefGoogle Scholar
  8. Vermeulen, R.C. and Cohen, M.H.: 1994, ApJ 430, 467.ADSCrossRefGoogle Scholar
  9. Tavecchio, E, Maraschi, L., Sambruna, R.M. and Urry, C.M.: 2000, ApJ 544, L23.ADSCrossRefGoogle Scholar
  10. Tóth, G.: 1996, Astrophys. Lett. Commun. 34, 245.ADSGoogle Scholar

Copyright information

© Springer Science+Business Media Dordrecht 2004

Authors and Affiliations

  • Rony Keppens
    • 1
  • Hubert Baty
    • 2
  • Jeroen Bergmans
    • 3
  • Fabien Casse
    • 1
  1. 1.FOM-Institute for Plasma Physics RijnhuizenAssociation Euratom/FOMNieuwegeinThe Netherlands
  2. 2.Observatoire AstronomiqueStrasbourgFrance
  3. 3.Astronomical InstituteUtrecht UniversityUtrechtThe Netherlands

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