Wandering Beam: Difference between revisions
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== Model Description == | == Model Description == | ||
FRBs may be formed by a scaled down version of an AGN . The jet formation and beaming mechanism is as in the AGN scenario, but the BH under consideration has a mass lower than the supermassive BHs of AGNs. If the moderately sized BH is set in a turbulent medium, such as a giant molecular cloud in a starburst galaxy, the angular momentum axis of the BH may be large, and the narrowly collimated beams will randomly change directions. When a beam sweeps across an observers line of sight, it may be observable as an FRB. There will be a persistent variable radio signal as in an AGN, and very soft X-ray/extreme UV emission from the accretion disk of the BH. The latter would be strongly absorbed in the Galactic plane, and thus only observable for FRBs at high Galactic latitudes. | |||
== Observational Constraints == | == Observational Constraints == | ||
Revision as of 05:00, 11 October 2018
| 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 | Wandering Beam | Repeat | -- | Synch. | Yes | -- | -- | -- | -- | Yes | -- | -- | -- | http://adsabs.harvard.edu/abs/2017MNRAS.471L..92K | None |
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
Model Description
FRBs may be formed by a scaled down version of an AGN . The jet formation and beaming mechanism is as in the AGN scenario, but the BH under consideration has a mass lower than the supermassive BHs of AGNs. If the moderately sized BH is set in a turbulent medium, such as a giant molecular cloud in a starburst galaxy, the angular momentum axis of the BH may be large, and the narrowly collimated beams will randomly change directions. When a beam sweeps across an observers line of sight, it may be observable as an FRB. There will be a persistent variable radio signal as in an AGN, and very soft X-ray/extreme UV emission from the accretion disk of the BH. The latter would be strongly absorbed in the Galactic plane, and thus only observable for FRBs at high Galactic latitudes.