Axion Cloud and BH - Revision history

Emma Platts at 08:57, 12 October 2018

2018-10-12T08:57:38Z

← Older revision		Revision as of 04:57, 12 October 2018
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	== Observational Constraints ==		== Observational Constraints ==

	Observational counterparts could be associated with ~~e+e−~~ annihilation and/or positronium (a bound particle of an e+ and e−), though these are not specified. GWs are also expected.		Observational counterparts could be associated with electron-positron annihilation and/or positronium (a bound particle of an electron and positron), though these are not specified. GWs are also expected.

Jake Gordin at 09:26, 11 October 2018

2018-10-11T09:26:18Z

← Older revision		Revision as of 05:26, 11 October 2018
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	\|GWCounterpart = Yes		\|GWCounterpart = Yes
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = ~~https~~://~~arxiv~~.~~org~~/~~pdf~~/1709.06581~~.pdf~~		\|References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1709.06581
	\|Comments = Observational counterparts could be associated with electron-positron annihilation and/or positronium.		\|Comments = Observational counterparts could be associated with electron-positron annihilation and/or positronium.
	}}		}}

Apw at 09:12, 10 October 2018

2018-10-10T09:12:07Z

← Older revision		Revision as of 05:12, 10 October 2018
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	== Model Description ==		== Model Description ==

	To be ~~filled~~ in with ~~updated draft~~		Spinning BHs have superradiant instabilities, and thus may be surrounded by a dense superradiant axion cloud. Similarly to how a laser can be generated by stimulated axion decay in dense axion clusters, a laser can be triggered in superradiant axion clusters. Such is known as a black hole laser powered by axion superradiant instabilities (BLAST). For a BLAST’s emission to be consistent with FRB observations, the required mass dictates that the BHs be primordial. However, because PBHs form when over densities of gas collapse, they do not have spin, and are unlikely to spin up via accretion. The merging of two PBHs is thus considered for FRBs, where the required spin and resultant superradiant instabilities can be induced. Repeating bursts could occur: the BLAST will form a photon plasma that blocks axion decay and thus halts lasing until e+/e− annihilation reduces the plasma density, and the process can restart.

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

	To be ~~filled in~~ with ~~updated draft~~		Observational counterparts could be associated with e+e− annihilation and/or positronium (a bound particle of an e+ and e−), though these are not specified. GWs are also expected.

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

2018-10-02T13:01:30Z

Created page with "   {{FRBTableTemplate |Category = Collision..."

New page

{{FRBTableTemplate
|Category = Collision / Interaction
|Progenitor = Superradiant Axion Cloud and BH
|Type = Repeat
|EnergyMechanism = Laser
|EmissionMechanism = Synch.
|LFRadioCounterpart = Yes
|HFRadioCounterpart = --
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = --
|XrayCounterpart = --
|GammarayCounterpart = --
|GWCounterpart = Yes
|NeutrinoCounterpart = --
|References = https://arxiv.org/pdf/1709.06581.pdf
|Comments = Observational counterparts could be associated with electron-positron annihilation and/or positronium.
}}

== Model Description ==

To be filled in with updated draft

== Observational Constraints ==

To be filled in with updated draft