Magnetic Field Amplification in M82 Winds Caused by Kelvin‐Helmholtz Modes
- 10 June 1999
- journal article
- research article
- Published by American Astronomical Society in The Astrophysical Journal
- Vol. 518 (1) , 177-182
- https://doi.org/10.1086/307273
Abstract
Halos of active galaxies can show relatively strong magnetic fields. Observations indicate that such halo fields, which are significantly stronger than one would expect from the disk field strengths, seem to be associated with the dynamical flows and winds in the halo. Numerical simulations show that unstable Kelvin-Helmholtz modes, which are common in a sheared plasma flow configuration, can cause the observed magnetic field amplification in the halo of the prototype starburst galaxy M82. This result comes out to be widely independent from the specific choice of dynamical parameters as long as the Kelvin-Helmholtz instability onset criterion is fulfilled.Keywords
This publication has 23 references indexed in Scilit:
- 3-D MHD simulations of extragalactic jetsPublished by Springer Nature ,2008
- The MHD Kelvin‐Helmholtz Instability. II. The Roles of Weak and Oblique Fields in Planar FlowsThe Astrophysical Journal, 1997
- The evolution of plane current–vortex sheetsPhysics of Plasmas, 1997
- Tearing instability, Kelvin‐Helmholtz instability, and magnetic reconnectionJournal of Geophysical Research, 1997
- The Magnetohydrodynamic Kelvin-Helmholtz Instability: A Two-dimensional Numerical StudyThe Astrophysical Journal, 1996
- Self-generation of magnetic fields by sheared flows in weakly ionized plasmasPhysics of Fluids B: Plasma Physics, 1993
- Magnetic fields in late-type galaxiesMonthly Notices of the Royal Astronomical Society, 1993
- Nonlinear dynamics of a three-dimensional jetThe Astrophysical Journal, 1992
- MHD Kelvin-Helmholtz instability in extended radio jetsThe Astrophysical Journal, 1984
- VLA radio continuum observations of the edge-on spiral galaxy NGC 3079The Astrophysical Journal, 1983