Magnetic flux paradigm for radio-loudness of AGN

TL;DR

This paper proposes that magnetic flux accumulation near black holes, rather than spin or accretion rate, primarily determines the radio-loudness of AGN, with different accretion phases influencing jet formation.

Contribution

It introduces the magnetic flux paradigm for AGN radio-loudness, emphasizing the role of flux accumulation during hot accretion phases and its impact on jet production.

Findings

Magnetic flux threading the black hole is key to jet launching.

Radio-loud quasars are linked to cold accretion following hot phases.

Flux accumulation can produce a magnetically choked accretion flow.

Abstract

We argue that the magnetic flux threading the black hole, rather than black hole spin or Eddington ratio, is the dominant factor in launching powerful jets and thus determining the radio loudness of active galactic nuclei (AGN). Most AGN are radio quiet because the thin accretion disks that feed them are inefficient in depositing magnetic flux close to the black hole. Flux accumulation is more likely to occur during a hot accretion (or thick disk) phase, and we argue that radio-loud quasars and strong emission-line radio galaxies occur only when a massive, cold accretion event follows an episode of hot accretion. Such an event might be triggered by the merger of a giant elliptical galaxy with a disk galaxy. This picture supports the idea that flux accumulation can lead to the formation of a so-called magnetically choked accretion flow (MCAF). The large observed range in radio loudness reflects not only the magnitude of the flux pressed against the black hole, but also the decrease in UV flux from the disk, due to its disruption by the "magnetosphere" associated with the accumulated flux. While the strongest jets result from the secular accumulation of flux, moderate jet activity can also be triggered by fluctuations in the magnetic flux deposited by turbulent, hot inner regions of otherwise thin accretion disks, or by the dissipation of turbulent fields in accretion disk coronae. These processes could be responsible for jet production in Seyferts and low-luminosity AGN, as well as jets associated with X-ray binaries.