KNBH-BH (Inspiral): Difference between revisions

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{{FRBTableTemplate
{{FRBTableTemplate
|Category              = Merger
|Category              = Merger
|Progenitor            = NS-NS
|Progenitor            = KNBH-BH
|Type                  = Single
|Type                  = Single
|EnergyMechanism        = Mag. flux change
|EnergyMechanism        = Mag. flux change
|EmissionMechanism      = Curv.
|EmissionMechanism      = Curv.
|LFRadioCounterpart    = Yes
|LFRadioCounterpart    = Yes
|HFRadioCounterpart    = --
|HFRadioCounterpart    = Afterglow
|MicrowaveCounterpart  = --
|MicrowaveCounterpart  = --
|THzCounterpart        = --
|THzCounterpart        = --
|OIRCounterpart        = --
|OIRCounterpart        = --
|XrayCounterpart        = Afterglow
|XrayCounterpart        = Yes
|GammarayCounterpart    = sGRB <br/> if jet aligned
|GammarayCounterpart    = sGRB <br/> if jet aligned
|GWCounterpart          = Yes
|GWCounterpart          = Yes
|NeutrinoCounterpart    = --
|NeutrinoCounterpart    = --
|References            = https://arxiv.org/pdf/1602.04542.pdf
|References            = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1602.04542
|Comments              = The estimated merger rate of binary BH systems is ~20 times smaller than that estimated for FRBs, and thus the theory can only account for the full population in the unlikely case that only <5% of FRBs are cosmological.
|Comments              = Unlikely to account for full FRB population.
}}
}}


== Model Description ==
== Model Description ==


A binary BH system in which at least one of the spinning BHs carries a charge would induce a global magnetic dipole normal to the orbital plane. During inspiral, as the orbital separation decreases, the magnetic flux of the system changes rapidly, which leads to particle bunching and the emission of coherent curvature radiation. And for some minimal values of the charge of the BH,  this scenario could produce an FRB and a sGRB \cite{Zhang:2016rli}. The detection of both signals could provide a lower limit on the charge, and the non-detection of a sGRB could provide an upper limit.
A binary BH system in which at least one of the spinning BHs carries a charge would induce a global magnetic dipole normal to the orbital plane. During inspiral, as the orbital separation decreases, the magnetic flux of the system changes rapidly, which leads to particle bunching and the emission of coherent curvature radiation.


== Observational Constraints ==
== Observational Constraints ==
For some minimal values of the charge of the BH, this scenario could produce an FRB and a sGRB. The detection of both signals could provide a lower limit on the charge, and the non-detection of a sGRB could provide an upper limit.

Latest revision as of 05:37, 11 October 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 KNBH-BH Single Mag. flux change Curv. Yes Afterglow -- -- -- Yes sGRB
if jet aligned
Yes -- http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1602.04542 Unlikely to account for full FRB population.

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


Model Description

A binary BH system in which at least one of the spinning BHs carries a charge would induce a global magnetic dipole normal to the orbital plane. During inspiral, as the orbital separation decreases, the magnetic flux of the system changes rapidly, which leads to particle bunching and the emission of coherent curvature radiation.

Observational Constraints

For some minimal values of the charge of the BH, this scenario could produce an FRB and a sGRB. The detection of both signals could provide a lower limit on the charge, and the non-detection of a sGRB could provide an upper limit.