NS-NS Merger (Mag. Braking): Difference between revisions
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== Observational Constraints == | == Observational Constraints == | ||
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Latest revision as of 06:27, 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 | |||||||
| Merger | NS-NS | Single | Mag. braking | -- | Yes | Yes | -- | -- | Kilonova | Afterglow | sGRB if jet aligned |
Yes | -- | http://adsabs.harvard.edu/abs/2013PASJ...65L..12T | |
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
Model Description
Consider the merging of two differentially rotating NSs into a uniformly rotating hypermassive NS. Upon coalescence, the merger spins down and magnetic braking generates coherent radiation. Since the merger rate of NSs is consistent with the expected FRB rate, this model implies that a large fraction of NS mergers must produce FRBs. Significant mass ejections are likely to occur during the merger process, which render FRBs unable to penetrate the ejecta. There is a 1 ms time frame after the maximum rotation speed of the merger is reached and before the release of dynamical ejecta, during which the transmission of a single FRB is possible.
Observational Constraints
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