Difference between revisions of "WD-BH Merger"

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|References            = http://adsabs.harvard.edu/abs/2018arXiv180804822P, http://adsabs.harvard.edu/abs/2018arXiv180804822P
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|References            = http://adsabs.harvard.edu/abs/2018RAA....18...61L
 
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== Model Description ==
 
== Model Description ==
  
A broader description, observational effects and detailed information.
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--To fill in with updated draft--
This is an FRB model where the merger of two neutron stars would lead to the generation of an isotropic radio pulse.
 
  
 
== Observational Constraints ==
 
== 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.
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Revision as of 03:38, 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
Merger WD-BH Single Maser Synch. -- -- -- -- -- Accretion disk -- -- -- http://adsabs.harvard.edu/abs/2018RAA....18...61L None

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


Model Description

--To fill in with updated draft--

Observational Constraints

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