Magnetohydrodynamic properties of extragalactic jets

• Published in: Astrophysics and space science Vol. 336; no. 1; pp. 15 - 19
• Main Authors: Nakamura, M., Meier, D. L., Garofalo, D.
• Format: Journal Article
• Language: English
• Published: Dordrecht Springer Netherlands 01.11.2011; Springer Nature B.V
• Subjects: Astrobiology; Astronomy; Astrophysics; Astrophysics and Astroparticles; Cosmology; Fluid mechanics; Jets; Magnetic fields; Numerical analysis; Observations and Techniques; Original Article; Physics; Physics and Astronomy; Space Exploration and Astronautics; Space Sciences (including Extraterrestrial Physics; Stars & galaxies; Active galaxies; MHD; Jets galaxies; Numerical methods
• ISSN: 0004-640X; 1572-946X
• DOI: 10.1007/s10509-010-0490-z

The theory that magnetic fields are instrumental in the formation and propagation of jets in active galactic nuclei dates back four decades. Despite a recent growing consensus on this notion stemming from the results of numerical simulations of magnetohydrodynamic (MHD) flows near black holes, the precise dynamical role of magnetic fields in observed parsec and kiloparsec jets remains uncertain. Some of the unanswered fundamental questions about extragalactic jets include the location where the flow becomes relativistic and where acceleration and collimation terminate, as well as the specifics of how the flow interacts with the ISM. Such observed properties as superluminal motions and wiggled structures based on numerical simulations to constitute the foundation of an MHD paradigm for extragalactic jets. We particularly focus our attention to the M87 jet, which is one of the best candidates to investigate relativistic outflows in extragalactic system.