Axion Minicluster and NS - Revision history

Emma Platts at 08:58, 12 October 2018

2018-10-12T08:58:46Z

← Older revision		Revision as of 04:58, 12 October 2018
Line 19:		Line 19:
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2015JETPL.101....1T		\|References = http://adsabs.harvard.edu/abs/2015JETPL.101....1T
	\|Comments = ~~The predicted emission timescale, the energetics, luminosities, and event rate are in-keeping with FRB observations.~~		\|Comments = None
	}}		}}

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

	Axion clumps with masses below the stellar range, known as Axion Bose Clusters or “miniclusters”, have been considered as FRB progenitors. In the strong magnetic field of a compact object, an instability may arise in a minicluster, causing it to explosively decay into photons via a synchrotron maser mechanism.		Axion clumps with masses below the stellar range, known as Axion Bose Clusters or “miniclusters”, have been considered as FRB progenitors. In the strong magnetic field of a compact object, an instability may arise in a minicluster, causing it to explosively decay into photons via a synchrotron maser mechanism. The predicted emission timescale, the energetics, luminosities, and event rate are in-keeping with FRB observations.

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

	--		--

Jake Gordin: /* Observational Constraints */

2018-10-11T10:40:03Z

Observational Constraints

← Older revision		Revision as of 06:40, 11 October 2018
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	== Observational Constraints ==		== Observational Constraints ==

			--

Jake Gordin at 10:39, 11 October 2018

2018-10-11T10:39:49Z

← Older revision		Revision as of 06:39, 11 October 2018
Line 19:		Line 19:
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2015JETPL.101....1T		\|References = http://adsabs.harvard.edu/abs/2015JETPL.101....1T
	\|Comments = ~~None~~		\|Comments = The predicted emission timescale, the energetics, luminosities, and event rate are in-keeping with FRB observations.
	}}		}}

Apw: /* Observational Constraints */

2018-10-10T09:42:23Z

Observational Constraints

← Older revision		Revision as of 05:42, 10 October 2018
Line 27:		Line 27:

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

	~~The predicted emission timescale, the energetics, luminosities, and event rate are in-keeping with FRB observations.~~

Apw: /* Observational Constraints */

2018-10-10T09:41:46Z

Observational Constraints

← Older revision		Revision as of 05:41, 10 October 2018
Line 28:		Line 28:
	== Observational Constraints ==		== Observational Constraints ==

	~~To be filled~~ in with ~~updated draft~~		The predicted emission timescale, the energetics, luminosities, and event rate are in-keeping with FRB observations.

Apw: /* Model Description */

2018-10-10T09:27:40Z

Model Description

← Older revision		Revision as of 05:27, 10 October 2018
Line 24:		Line 24:
	== Model Description ==		== Model Description ==

	Axion clumps with masses below the stellar range, known as Axion Bose Clusters or ~~“miniclus- ters”~~, have been considered as FRB progenitors. In the strong magnetic field of a compact object, an instability may arise in a minicluster, causing it to explosively decay into photons via a synchrotron maser mechanism.		Axion clumps with masses below the stellar range, known as Axion Bose Clusters or “miniclusters”, have been considered as FRB progenitors. In the strong magnetic field of a compact object, an instability may arise in a minicluster, causing it to explosively decay into photons via a synchrotron maser mechanism.

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

	To be filled in with updated draft		To be filled in with updated draft

Apw: /* Model Description */

2018-10-10T09:27:11Z

Model Description

← Older revision		Revision as of 05:27, 10 October 2018
Line 24:		Line 24:
	== Model Description ==		== Model Description ==

	~~To be filled~~ in ~~with updated draft~~		Axion clumps with masses below the stellar range, known as Axion Bose Clusters or “miniclus- ters”, have been considered as FRB progenitors. In the strong magnetic field of a compact object, an instability may arise in a minicluster, causing it to explosively decay into photons via a synchrotron maser mechanism.

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

	To be filled in with updated draft		To be filled in with updated draft

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

2018-10-02T12:56:51Z

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

New page

{{FRBTableTemplate
|Category = Collision / Interaction
|Progenitor = Axion Minicluster and NS
|Type = Single
|EnergyMechanism = Maser
|EmissionMechanism = Synch.
|LFRadioCounterpart = Yes
|HFRadioCounterpart = --
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = --
|XrayCounterpart = --
|GammarayCounterpart = --
|GWCounterpart = --
|NeutrinoCounterpart = --
|References = http://adsabs.harvard.edu/abs/2015JETPL.101....1T
|Comments = None
}}

== Model Description ==

To be filled in with updated draft

== Observational Constraints ==

To be filled in with updated draft