Wandering Pulsar: Difference between revisions
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|GWCounterpart = -- | |GWCounterpart = -- | ||
|NeutrinoCounterpart = -- | |NeutrinoCounterpart = -- | ||
|References = | |References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1611.01243 | ||
|Comments = Any counterparts will be associated with the pulsar, but are not specified. | |Comments = Any counterparts will be associated with the pulsar, but are not specified. | ||
}} | }} | ||
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== Model Description == | == Model Description == | ||
This model assumes the presence of a steady beam of pulsar emission whose | This model assumes the presence of a steady beam of pulsar emission whose direction 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 == | ||
This scenario can also consistently explain two pairs of possibly distinct radio bursts detected in FRB 121102. Details about an emission mechanism or possible counterparts are not given. | |||
Latest revision as of 10:58, 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 | |||||||
| Other | Wandering Pulsar Beams | Repeat | -- | -- | Yes | -- | -- | -- | -- | -- | -- | -- | -- | http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1611.01243 | 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 direction 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
This scenario can also consistently explain two pairs of possibly distinct radio bursts detected in FRB 121102. Details about an emission mechanism or possible counterparts are not given.