AGN-KBH
| Category | Progenitor | Type | Energy Mechanism | Emission Mechanism | Counterparts | References | Brief Comments | ||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| LF Radio | HF Radio | Microwave | Terahertz | Optical/IR | X-rays | Gamma-rays | Gravitational Waves | Neutrinos | |||||||
| AGN | AGN-KBH Interaction | Repeat | Maser | Synch. | Yes | -- | -- | -- | Supernova | -- | Yes | Yes | Yes | http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1709.00185 | Neutrinos from preceding SN and from collapse to BH. |
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
Model Description
Episodic winds from an AGN may prompt a KBH to intermittently accrete matter, producing a repeating FRB. Through the Blandford-Znajek mechanism, in which a magnetic field extracts spin energy from the KBH, an unsteady bipolar jet is triggered. As the jet travels through the surrounding plasma, shocked shells create a synchrotron maser.
Observational Constraints
The KBH under consideration may form via a series of events: the collapse of a Wolf-Rayet star (a relatively small helium star) into a supramassive magnetar that accretes matter until it collapses into a KBH. Precursors to the FRB may therefore be the SN Type Ib/c explosion in which the magnetar was born, and the resultant neutrinos and gravitational waves. The release of a prompt GRB may also be observable as the magnetar spins down, but only if the axis of the magnetar is aligned with earth. Gravitational waves will also occur when the magnetar implodes to a quark star.