Template:NewFRBModel: Difference between revisions
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|NeutrinoCounterpart = Not detectable | |NeutrinoCounterpart = Not detectable | ||
|Reference = http://adsabs.harvard.edu/abs/2018arXiv180804822P | |Reference = http://adsabs.harvard.edu/abs/2018arXiv180804822P | ||
|Comments = | |Comments = None | ||
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Revision as of 17:25, 24 September 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 | |||||||
| Merger | NS-NS | Non-repeating | Mag. reconnection | Curv. | Yes (excluding self absorption) | Maybe | Maybe | No | Afterglow | Yes, if jet aligned | Yes | Not detectable | None | ||
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
Model Description
A broader description, observational effects and detailed information. This is an FRB model where the merger of two neutron stars would lead to the generation of an isotropic radio pulse.
Observational Constraints
In general this model would predict that FRBs arise from old stellar populations where NS-NS binary systems have had time to form and evolve into compact orbits.