Wandering Beam: Difference between revisions
Emma Platts (talk | contribs) No edit summary |
|||
| (One intermediate revision by the same user not shown) | |||
| Line 23: | Line 23: | ||
== 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 == | ||
- | |||
Latest revision as of 06:25, 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.
Observational Constraints
-