Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.0801n&link_type=abstract
2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #08.01; Bulletin of the American Astronomical Society, V
Astronomy and Astrophysics
Astronomy
Scientific paper
Propagation of "magnetic tower'' jets in gravitationally stratified atmospheres in large scales (> tens of kpc) has been examined by performing three-dimensional magnetohydrodynamic (MHD) simulations. The MHD wave structures, the cylindrical radial force balance, and the stability properties of magnetic tower jets will be discussed based on the nonlinear solutions. During the dynamical evolution of magnetic towers, the narrow "jet body'' and the expanded "lobe'', both of which are magnetically dominated, are formed. In our results, a preceding hydrodynamic shock, which may be identified as an AGN-driven shock in X-ray observation, plays an important role in the dynamics of magnetic towers. A strong compression at the head of tower front and radial collimation to produce a slender-shaped jet are observed. The axial jet current and the external gas pressure can determine the width of radio lobes. The current-carrying, Poynting flux-dominated magnetic tower jet, which possesses a highly wound helical magnetic field, is subject to the current-driven instability (CDI). We find that the propagating magnetic tower jets develop the non-axisymmetric mode of the CDI. Both the internal elliptical (m=2) mode like the "double helix'' and the external kink (m=1) mode to form the large scale wiggles grow in different parts of magnetic towers. The pressure-driven and shear-driven instabilities do not occur in the magnetic tower jets. This strongly suggests that the CDI is the primary reason to determine the large scale structure in AGN jets.
Li Handong
Nakamura Masanori
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