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4 - The Role of Magnetic Fields in AGN Activity and Feedback

Published online by Cambridge University Press:  21 April 2018

By
Rony Keppens ,
Oliver Porth  and
Hans J. P. Goedbloed
Edited by
Jorge Sánchez Almeida  and
María Jesús Martínez González
Rony Keppens
Affiliation:
KU Leuven, Belgium
Oliver Porth
Affiliation:
KU Leuven, Belgium & School of Mathematics, University of Leeds,
Hans J. P. Goedbloed
Affiliation:
FOM Institute DIFFER, Nieuwegein, The Netherlands
Jorge Sánchez Almeida
Affiliation:
Instituto de Astrofísica de Canarias, Tenerife
María Jesús Martínez González
Affiliation:
Instituto de Astrofísica de Canarias, Tenerife
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Summary

Abstract

Active galactic nuclei (AGNs), the luminous, compact core regions of galaxies where accretion occurs onto supermassive black holes, can dramatically influence their entire host galaxy evolution by a process referred to as AGN feedback. Energy feedback to the galaxy is the result of combined radiation fields and directed outflows, and especially radio-loud active galaxies show pronounced jets and lobes. Their synchrotron radio emission indicates that dynamically important magnetic fields are at play in AGN jet collimation, stability, energy transfer to the intergalactic medium and their overall morphological appearance. Current knowledge on the launching mechanisms for such highly energetic relativistic jets, as well as the near black-hole accretion processes themselves, all invoke magnetic fields as active agents in angular momentum, mass and energy redistributions. In this review, we cover aspects of AGN feedback and the role played by magnetic fields, almost necessarily studied at vastly different length and timescales. We emphasize how typical large-scale galaxy interaction studies rely on parametric prescriptions for feedback, while detailed dedicated studies for near black-hole dynamics and relativistic jet propagation exist which take full account of magnetic field influences. We discuss representative hydro to magnetohydrodynamic (MHD) numerical simulations that exploit analogies with less energetic X-ray binary sources or even protostellar accretion-ejection systems, emphasize relativistic MHD descriptions, and point out that magnetic fields in accretion disks yield many linear instability routes to turbulence that have scarcely been recognized in the astrophysical community. In combination, they serve to show that magnetic field influences in AGN accretion, jet launch, energy feedback, and overall evolution are still far from completely understood, although many aspects have been disclosed by advanced analytical and numerical relativistic MHD studies.

Motivation: Astrophysical Jets

Radio galaxies confront us with dramatic views on energy redistributions at all scales, as mediated by central massive black holes lurking in their nucleus. A clear example is provided by the elliptical galaxy NGC5532, a nearby (red shift z = 0.0237, type S0) galaxy where the stellar distribution is in sharp contrast with its double-jetted appearance in radio images.

Type
Chapter
Information
Cosmic Magnetic Fields
, pp. 87 - 122
Publisher: Cambridge University Press
Print publication year: 2018

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