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.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
