Difference between revisions of "Template:NewFRBModel"

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|GWCounterpart          = Yes
 
|GWCounterpart          = Yes
 
|NeutrinoCounterpart    = Not detectable
 
|NeutrinoCounterpart    = Not detectable
|Reference              = http://adsabs.harvard.edu/abs/2018arXiv180804822P
+
|References            = http://adsabs.harvard.edu/abs/2018arXiv180804822P, http://adsabs.harvard.edu/abs/2018arXiv180804822P
 
|Comments              = None
 
|Comments              = None
 
}}
 
}}

Revision as of 11:43, 25 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
Merger NS-NS Non-repeating Mag. reconnection Curv. Yes (excluding self absorption) Yes Maybe Maybe No Afterglow Yes, if jet aligned Yes Not detectable http://adsabs.harvard.edu/abs/2018arXiv180804822P, http://adsabs.harvard.edu/abs/2018arXiv180804822P None

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


Model Description

A broader description, observational effects and detailed information. This is an FRB model where the merger of two neutron stars would lead to the generation of an isotropic radio pulse.

Observational Constraints

In general this model would predict that FRBs arise from old stellar populations where NS-NS binary systems have had time to form and evolve into compact orbits.