Jet-Caviton: Difference between revisions
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|GWCounterpart = Yes | |GWCounterpart = Yes | ||
|NeutrinoCounterpart = -- | |NeutrinoCounterpart = -- | ||
|References = http://adsabs.harvard.edu/abs/2016PhRvD..93b3001R, | |References = http://adsabs.harvard.edu/abs/2016PhRvD..93b3001R, http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1704.08097 | ||
|Comments = | |Comments = Persistent scintillating radio emission. | ||
}} | }} | ||
== Model Description == | == Model Description == | ||
A hot accretion disk forms as matter is captured and spirals into a moderately sized BH. Some of the in-falling gas and dust is confined to the poles and ejected in two relativistic jets. Hot gas clouds of varying densities surround the BH, forming a toroid that extends a few parsecs from the BH. As the AGN jet interacts with the clouds, it becomes narrowly collimated. The relativistic electron-positron beam encounters material at the center of the host galaxy, and strong turbulence is produced by plasma instabilities. The total pressure and the ponderomotive force (experienced by a charged particle in an oscillating electric field) cause electrons and ions to separate. These regions, called cavitons, are filled by a strong electrostatic field. Electrons from the beam that pass through the caviton are coherently scattered and emit strongly beamed Bremsstrahlung radiation in pulses. FRBs may be single or repeating. | |||
== Observational Constraints == | == Observational Constraints == | ||
Radiation might be linearly polarized if there is a local magnetic field, however the 100% polarization degree of FRB 121102 would be difficult to account for in this scenario. The persistent scintillating radio emission from the AGN is an expected counterpart, which agrees with observations of FRB 121102. | Radiation might be linearly polarized if there is a local magnetic field, however the 100% polarization degree of FRB 121102 would be difficult to account for in this scenario. The persistent scintillating radio emission from the AGN is an expected counterpart, which agrees with observations of FRB 121102. | ||
Latest revision as of 06:05, 15 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 | Jet-Caviton Interaction | Both | Electron scattering | Bremsst. | Yes | Yes | -- | -- | -- | -- | Possible GRB | Yes | -- | http://adsabs.harvard.edu/abs/2016PhRvD..93b3001R, http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1704.08097 | Persistent scintillating radio emission. |
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
Model Description
A hot accretion disk forms as matter is captured and spirals into a moderately sized BH. Some of the in-falling gas and dust is confined to the poles and ejected in two relativistic jets. Hot gas clouds of varying densities surround the BH, forming a toroid that extends a few parsecs from the BH. As the AGN jet interacts with the clouds, it becomes narrowly collimated. The relativistic electron-positron beam encounters material at the center of the host galaxy, and strong turbulence is produced by plasma instabilities. The total pressure and the ponderomotive force (experienced by a charged particle in an oscillating electric field) cause electrons and ions to separate. These regions, called cavitons, are filled by a strong electrostatic field. Electrons from the beam that pass through the caviton are coherently scattered and emit strongly beamed Bremsstrahlung radiation in pulses. FRBs may be single or repeating.
Observational Constraints
Radiation might be linearly polarized if there is a local magnetic field, however the 100% polarization degree of FRB 121102 would be difficult to account for in this scenario. The persistent scintillating radio emission from the AGN is an expected counterpart, which agrees with observations of FRB 121102.