Wandering Pulsar: Difference between revisions
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Emma Platts (talk | contribs) (Created page with " <!-- Brings in the summary table --> <!-- This is an example. Change the right hand side of all these assignments --> {{FRBTableTemplate |Category = Other |Pro...") |
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== Model Description == | == Model Description == | ||
This model assumes the presence of a steady beam of pulsar emission whose directly randomly changes. If this beam sweeps across the line of sight of an observer, it may be observable as an FRB. The duration of the FRB depends on the speed at which the beam moves across the sky, and hence a wandering beam mitigates the enormous power and high spin-down requirements of giant pulse and flare models. | |||
== Observational Constraints == | == Observational Constraints == | ||
To be filled in with updated draft | To be filled in with updated draft | ||
Revision as of 06:09, 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 | Wandering Pulsar Beams | Repeat | -- | -- | Yes | -- | -- | -- | -- | -- | -- | -- | -- | https://arxiv.org/pdf/1611.01243.pdf | Any counterparts will be associated with the pulsar, but are not specified. |
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
Model Description
This model assumes the presence of a steady beam of pulsar emission whose directly randomly changes. If this beam sweeps across the line of sight of an observer, it may be observable as an FRB. The duration of the FRB depends on the speed at which the beam moves across the sky, and hence a wandering beam mitigates the enormous power and high spin-down requirements of giant pulse and flare models.
Observational Constraints
To be filled in with updated draft