Young Magnetars: Difference between revisions
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== Model Description == | == Model Description == | ||
This model considers FRBs from magnetars born in NS-NS mergers and accretion induced WD collapse. The FRBs themselves are formed by the same mechanism as that of giant flare FRB theories. | |||
== Observational Constraints == | == Observational Constraints == | ||
FRBs from magnetars born in NS-NS mergers and accretion induced WD collapse will be accompanied by persistent synchrotron radio emissionon timescales of months to years, powered by the nebula of relativistic electrons and magnetic fields inflated by the magnetar flares, or on longer timescales through interaction of the merger ejecta with the interstellar medium; this timescale is shorter than for the SLSN/LGRB channel. | |||
Revision as of 08:14, 6 September 2019
| 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/Collapse | Magnetars Born in NS-NS Mergers and WD Collapse | Repeat | Maser | Synch. | Yes (excl. self absorption) |
Yes | Maybe | Maybe | No | Afterglow | Yes if jet aligned |
Yes | Not detectable | https://arxiv.org/pdf/1907.00016.pdf | Same mechanisms as flares, but magnetars born in mergers or collapse as opposed in to SLSNe or LGRBs. |
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
Model Description
This model considers FRBs from magnetars born in NS-NS mergers and accretion induced WD collapse. The FRBs themselves are formed by the same mechanism as that of giant flare FRB theories.
Observational Constraints
FRBs from magnetars born in NS-NS mergers and accretion induced WD collapse will be accompanied by persistent synchrotron radio emissionon timescales of months to years, powered by the nebula of relativistic electrons and magnetic fields inflated by the magnetar flares, or on longer timescales through interaction of the merger ejecta with the interstellar medium; this timescale is shorter than for the SLSN/LGRB channel.