KNBH-BH (Inspiral) - Revision history

Jake Gordin at 09:37, 11 October 2018

2018-10-11T09:37:24Z

← Older revision		Revision as of 05:37, 11 October 2018
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	\|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 = Unlikely to account for full FRB population.		\|Comments = Unlikely to account for full FRB population.
	}}		}}

Apw: /* Observational Constraints */

2018-10-10T10:56:52Z

Observational Constraints

← Older revision		Revision as of 06:56, 10 October 2018
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	== 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.

Apw: /* Model Description */

2018-10-10T10:56:27Z

Model Description

← Older revision		Revision as of 06:56, 10 October 2018
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	== 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 ==

Emma Platts at 14:43, 26 September 2018

2018-09-26T14:43:24Z

← Older revision		Revision as of 10:43, 26 September 2018
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	\|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

Emma Platts at 14:40, 26 September 2018

2018-09-26T14:40:59Z

← Older revision		Revision as of 10:40, 26 September 2018
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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

Emma Platts at 14:39, 26 September 2018

2018-09-26T14:39:25Z

← Older revision		Revision as of 10:39, 26 September 2018
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	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = https://arxiv.org/pdf/1602.04542.pdf		\|References = https://arxiv.org/pdf/1602.04542.pdf
	\|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.
	}}		}}

Emma Platts: Created page with " {{FRBTableTemplate |Category = Merger |Pr..."

2018-09-26T14:38:28Z

Created page with "   {{FRBTableTemplate |Category = Merger |Pr..."

New page

{{FRBTableTemplate
|Category = Merger
|Progenitor = NS-NS
|Type = Single
|EnergyMechanism = Mag. flux change
|EmissionMechanism = Curv.
|LFRadioCounterpart = Yes
|HFRadioCounterpart = --
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = --
|XrayCounterpart = Afterglow
|GammarayCounterpart = sGRB <br/> if jet aligned
|GWCounterpart = Yes
|NeutrinoCounterpart = --
|References = https://arxiv.org/pdf/1602.04542.pdf
|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.
}}

== 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.

== Observational Constraints ==