Difference between revisions of "NS to KNBH"

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|GWCounterpart          = Yes
 
|GWCounterpart          = Yes
 
|NeutrinoCounterpart    = --
 
|NeutrinoCounterpart    = --
|References            = https://arxiv.org/pdf/1307.1409.pdf,  
+
|References            = https://arxiv.org/abs/1307.1409.pdf, https://arxiv.org/abs/1603.05509
 
|Comments              = Possible X-ray afterglow and a short/long GRB created in NS birth prior to the FRB.
 
|Comments              = Possible X-ray afterglow and a short/long GRB created in NS birth prior to the FRB.
 
}}
 
}}

Revision as of 14:07, 26 September 2018





Summary Table
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
Collapse NS to KNBH Single Mag. reconnection Curv. Yes -- -- -- -- -- -- Yes -- https://arxiv.org/abs/1307.1409.pdf, https://arxiv.org/abs/1603.05509 Possible X-ray afterglow and a short/long GRB created in NS birth prior to the FRB.

Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)


Model Description

Upon the collapse of a supramassive NS into a NKBH, an event horizon will likely form before most of the mass and radiation can escape. By the no-hair theorem, magnetic fields are forbidden from piercing the event horizon, and so the magnetosphere will be left behind. Alternatively, if a NS collapses into a metastable KNBH, its electric discharge can cause the magnetosphere to be shed. Violent magnetic reconnection outside the horizon would then induce a strong magnetic shock wave that moves through the remaining plasma at the speed of light, resulting in a single FRB.

Observational Constraints