AGN-SS - Revision history

Emma Platts at 08:55, 12 October 2018

2018-10-12T08:55:18Z

← Older revision		Revision as of 04:55, 12 October 2018
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	\|GWCounterpart = Yes		\|GWCounterpart = Yes
	\|NeutrinoCounterpart = Yes		\|NeutrinoCounterpart = Yes
	\|References = [http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1709.00185]		\|References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1709.00185
	\|Comments = Neutrinos from preceding SN and from collapse to BH. GW from collapse and persistent GWs from SS.		\|Comments = Neutrinos from preceding SN and from collapse to BH. GW from collapse and persistent GWs from SS.
	}}		}}

Shriharsh at 21:42, 11 October 2018

2018-10-11T21:42:35Z

← Older revision		Revision as of 17:42, 11 October 2018
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	\|GWCounterpart = Yes		\|GWCounterpart = Yes
	\|NeutrinoCounterpart = Yes		\|NeutrinoCounterpart = Yes
	\|References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1709.00185		\|References = [http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1709.00185]
	\|Comments = Neutrinos from preceding SN and from collapse to BH. GW from collapse and persistent GWs from SS.		\|Comments = Neutrinos from preceding SN and from collapse to BH. GW from collapse and persistent GWs from SS.
	}}		}}

Jake Gordin at 10:33, 11 October 2018

2018-10-11T10:33:22Z

← Older revision		Revision as of 06:33, 11 October 2018
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	== Model Description ==		== Model Description ==

	A strange quark star (SS) is made up of approximately the same number of up, down, and strange quarks, with a small number of electrons distributed across the star's surface. Should an AGN wind interact with a SS, it can induce torsional oscillation of the electron layer relative to the positively charged SS, which can emit high luminosity GHz radio waves ~~\cite{Mannarelli:2014jfa}~~, consistent with FRBs ~~\cite{DasGupta:2017uac}~~. The sporadic nature of AGN wind would induce a repeating FRB. Persistent gravitational waves are expected from the SS due to its r-mode instability \cite{Andersson:2001ev}. If the SS is the result of a spinning down magnetar, neutrinos and a GW could be released when the magnetar collapses, however this emission need not be close in time to the interaction of the SS with the AGN, making it difficult to draw any associations.		A strange quark star (SS) is made up of approximately the same number of up, down, and strange quarks, with a small number of electrons distributed across the star's surface. Should an AGN wind interact with a SS, it can induce torsional oscillation of the electron layer relative to the positively charged SS, which can emit high luminosity GHz radio waves, consistent with FRBs. The sporadic nature of AGN wind would induce a repeating FRB.

	== Observational Constraints ==		== Observational Constraints ==

			Persistent gravitational waves are expected from the SS due to its r-mode instability. If the SS is the result of a spinning down magnetar, neutrinos and a GW could be released when the magnetar collapses, however this emission need not be close in time to the interaction of the SS with the AGN, making it difficult to draw any associations.

Jake Gordin at 10:32, 11 October 2018

2018-10-11T10:32:16Z

← Older revision		Revision as of 06:32, 11 October 2018
Line 24:		Line 24:
	== Model Description ==		== Model Description ==

	* to ~~add~~		A strange quark star (SS) is made up of approximately the same number of up, down, and strange quarks, with a small number of electrons distributed across the star's surface. Should an AGN wind interact with a SS, it can induce torsional oscillation of the electron layer relative to the positively charged SS, which can emit high luminosity GHz radio waves \cite{Mannarelli:2014jfa}, consistent with FRBs \cite{DasGupta:2017uac}. The sporadic nature of AGN wind would induce a repeating FRB. Persistent gravitational waves are expected from the SS due to its r-mode instability \cite{Andersson:2001ev}. If the SS is the result of a spinning down magnetar, neutrinos and a GW could be released when the magnetar collapses, however this emission need not be close in time to the interaction of the SS with the AGN, making it difficult to draw any associations.

	== Observational Constraints ==		== Observational Constraints ==

Jake Gordin at 08:53, 11 October 2018

2018-10-11T08:53:56Z

← Older revision		Revision as of 04:53, 11 October 2018
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	\|GWCounterpart = Yes		\|GWCounterpart = Yes
	\|NeutrinoCounterpart = Yes		\|NeutrinoCounterpart = Yes
	\|References = ~~https~~://~~arxiv~~.~~org~~/~~pdf~~/1709.00185~~.pdf~~		\|References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1709.00185
	\|Comments = Neutrinos from preceding SN and from collapse to BH. GW from collapse and persistent GWs from SS.		\|Comments = Neutrinos from preceding SN and from collapse to BH. GW from collapse and persistent GWs from SS.
	}}		}}

Emma Platts at 14:48, 27 September 2018

2018-09-27T14:48:18Z

← Older revision		Revision as of 10:48, 27 September 2018
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	\|Type = Repeat		\|Type = Repeat
	\|EnergyMechanism = Electron oscillation		\|EnergyMechanism = Electron oscillation
	\|EmissionMechanism = ~~Open Question~~		\|EmissionMechanism = --
	\|LFRadioCounterpart = Yes		\|LFRadioCounterpart = Yes
	\|HFRadioCounterpart = --		\|HFRadioCounterpart = --

Emma Platts: Created page with " {{FRBTableTemplate |Category = AGN |Proge..."

2018-09-27T14:27:05Z

Created page with "   {{FRBTableTemplate |Category = AGN |Proge..."

New page

{{FRBTableTemplate
|Category = AGN
|Progenitor = AGN-Strange Star Interaction
|Type = Repeat
|EnergyMechanism = Electron oscillation
|EmissionMechanism = Open Question
|LFRadioCounterpart = Yes
|HFRadioCounterpart = --
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = Thermal
|XrayCounterpart = --
|GammarayCounterpart = Yes
|GWCounterpart = Yes
|NeutrinoCounterpart = Yes
|References = https://arxiv.org/pdf/1709.00185.pdf
|Comments = Neutrinos from preceding SN and from collapse to BH. GW from collapse and persistent GWs from SS.
}}

== Model Description ==

* to add

== Observational Constraints ==