Pulsar Lightning: Difference between revisions
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== Observational Constraints == | == Observational Constraints == | ||
The large variation of FRB 121102 burst widths, and hence the variation of spectra fluences and frequencies, are consistent with this model. | |||
Latest revision as of 06:02, 9 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 | |||||||
| Other | Pulsar Lightning | Repeat | Electrostatic | Curv. | Yes | -- | -- | -- | -- | -- | -- | -- | -- | http://adsabs.harvard.edu/abs/2017MNRAS.469L..39K | None |
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
Model Description
Akin to SGRs powered by the release magnetic energy stored in magnetars, FRBs may be powered by the release of electrostatic energy stored in pulsars. Provided there are regions of magnetospheric plasma with distinct energy, separated by a vacuum gap, the discharge of such energy could manifest as “pulsar lighting”, analogous to the flow of current in the atmosphere when lightning strikes. This intense, rapidly varying, electric field in the gaps would accelerate electrons and positrons in the magnetosphere, producing coherent curvature radiation observable as an FRB.
Observational Constraints
The large variation of FRB 121102 burst widths, and hence the variation of spectra fluences and frequencies, are consistent with this model.