MWN Shock (Single Flare): Difference between revisions
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|MicrowaveCounterpart = -- | |MicrowaveCounterpart = -- | ||
|THzCounterpart = -- | |THzCounterpart = -- | ||
|OIRCounterpart = | |OIRCounterpart = Maybe | ||
|XrayCounterpart = -- | |XrayCounterpart = -- | ||
|GammarayCounterpart = | |GammarayCounterpart = Low energy gamma-rays, sGRB if jet aligned | ||
|GWCounterpart = Yes | |GWCounterpart = Yes | ||
|NeutrinoCounterpart = -- | |NeutrinoCounterpart = -- | ||
|References = http://adsabs.harvard.edu/abs/2010vaoa.conf..129P, http://adsabs.harvard.edu/abs/2014MNRAS.442L...9L, http://adsabs.harvard.edu/abs/2017MNRAS.467.3542M | |References = http://adsabs.harvard.edu/abs/2010vaoa.conf..129P,http://adsabs.harvard.edu/abs/2014MNRAS.442L...9L,http://adsabs.harvard.edu/abs/2017MNRAS.467.3542M | ||
|Comments = None | |Comments = None | ||
}} | }} | ||
Latest revision as of 18:56, 12 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 | |||||||
| SNR (Magnetars) | MWD Shock (Single Flare) | Single | Maser | Synch. | Yes | Afterglow | -- | -- | Maybe | -- | Low energy gamma-rays, sGRB if jet aligned | Yes | -- | http://adsabs.harvard.edu/abs/2010vaoa.conf..129P,http://adsabs.harvard.edu/abs/2014MNRAS.442L...9L,http://adsabs.harvard.edu/abs/2017MNRAS.467.3542M | None |
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
Model Description
One of the first postulations for the Lorimer burst was a magnetar hyperflare. Since then the idea has been widely considered and built upon. An FRB model analogous to the pulsar wind bubble model above has been proposed, with the power now deriving from the magnetic energy of a magnetar, and the shock resulting from a giant flare impacting a magnetar wind nebula (MWN). A powerful synchrotron maser consistent with FRBs is formed at the termination shock, either by magnetic reconnection or a ring-like distribution of gyrating particles at the shock front.
Observational Constraints
Emission is expected to have a hump in the nebula spectrum near the nebula's self-absorption frequency.