MWN Shock (Single Flare) - Revision history

Shriharsh at 23:56, 12 October 2018

2018-10-12T23:56:21Z

← Older revision		Revision as of 19:56, 12 October 2018
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	\|GWCounterpart = Yes		\|GWCounterpart = Yes
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2010vaoa.conf..129P, http://adsabs.harvard.edu/abs/2014MNRAS.442L...9L, http://adsabs.harvard.edu/abs/2017MNRAS.467.3542M		\|References = http://adsabs.harvard.edu/abs/2010vaoa.conf..129P,http://adsabs.harvard.edu/abs/2014MNRAS.442L...9L,http://adsabs.harvard.edu/abs/2017MNRAS.467.3542M
	\|Comments = None		\|Comments = None
	}}		}}

Emma Platts at 13:00, 27 September 2018

2018-09-27T13:00:43Z

← Older revision		Revision as of 09:00, 27 September 2018
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	\|MicrowaveCounterpart = --		\|MicrowaveCounterpart = --
	\|THzCounterpart = --		\|THzCounterpart = --
	\|OIRCounterpart = --		\|OIRCounterpart = Maybe
	\|XrayCounterpart = --		\|XrayCounterpart = --
	\|GammarayCounterpart = ~~HEGF~~, sGRB if jet aligned		\|GammarayCounterpart = Low energy gamma-rays, sGRB if jet aligned
	\|GWCounterpart = Yes		\|GWCounterpart = Yes
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --

Emma Platts at 12:50, 27 September 2018

2018-09-27T12:50:27Z

← Older revision		Revision as of 08:50, 27 September 2018
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	\|OIRCounterpart = --		\|OIRCounterpart = --
	\|XrayCounterpart = --		\|XrayCounterpart = --
	\|GammarayCounterpart = HEGF, sGRB if aligned		\|GammarayCounterpart = HEGF, sGRB if jet aligned
	\|GWCounterpart = Yes		\|GWCounterpart = Yes
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --

Emma Platts at 12:49, 27 September 2018

2018-09-27T12:49:35Z

← Older revision		Revision as of 08:49, 27 September 2018
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	\|OIRCounterpart = --		\|OIRCounterpart = --
	\|XrayCounterpart = --		\|XrayCounterpart = --
	\|GammarayCounterpart = HEGF, sGRB ~~<br\>~~ if aligned		\|GammarayCounterpart = HEGF, sGRB if aligned
	\|GWCounterpart = Yes		\|GWCounterpart = Yes
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --

Emma Platts at 12:47, 27 September 2018

2018-09-27T12:47:44Z

← Older revision		Revision as of 08:47, 27 September 2018
Line 15:		Line 15:
	\|OIRCounterpart = --		\|OIRCounterpart = --
	\|XrayCounterpart = --		\|XrayCounterpart = --
	\|GammarayCounterpart = ~~Yes~~		\|GammarayCounterpart = HEGF, sGRB <br\> if aligned
	\|GWCounterpart = Yes		\|GWCounterpart = Yes
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --

Emma Platts at 12:44, 27 September 2018

2018-09-27T12:44:03Z

← Older revision		Revision as of 08:44, 27 September 2018
Line 18:		Line 18:
	\|GWCounterpart = Yes		\|GWCounterpart = Yes
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2010vaoa.conf..129P, http://adsabs.harvard.edu/abs/2014MNRAS.442L...9L,http://adsabs.harvard.edu/abs/2017MNRAS.467.3542M		\|References = http://adsabs.harvard.edu/abs/2010vaoa.conf..129P, http://adsabs.harvard.edu/abs/2014MNRAS.442L...9L, http://adsabs.harvard.edu/abs/2017MNRAS.467.3542M
	\|Comments = None		\|Comments = None
	}}		}}

Emma Platts: Created page with " {{FRBTableTemplate |Category = SNR (Magne..."

2018-09-27T12:32:37Z

Created page with "   {{FRBTableTemplate |Category = SNR (Magne..."

New page

{{FRBTableTemplate
|Category = SNR (Magnetars)
|Progenitor = MWD Shock (Single Flare)
|Type = Single
|EnergyMechanism = Maser
|EmissionMechanism = Synch.
|LFRadioCounterpart = Yes
|HFRadioCounterpart = Afterglow
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = --
|XrayCounterpart = --
|GammarayCounterpart = Yes
|GWCounterpart = Yes
|NeutrinoCounterpart = --
|References = http://adsabs.harvard.edu/abs/2010vaoa.conf..129P, http://adsabs.harvard.edu/abs/2014MNRAS.442L...9L,http://adsabs.harvard.edu/abs/2017MNRAS.467.3542M
|Comments = None
}}

== Model Description ==

One of the first postulations for the Lorimer burst was a magnetar hyperflare. Since then the idea has been widely considered and built upon. An FRB model analogous to the pulsar wind bubble model above has been proposed, with the power now deriving from the magnetic energy of a magnetar, and the shock resulting from a giant flare impacting a magnetar wind nebula (MWN). A powerful synchrotron maser consistent with FRBs is formed at the termination shock, either by magnetic reconnection or a ring-like distribution of gyrating particles at the shock front.

== Observational Constraints ==

Emission is expected to have a hump in the nebula spectrum near the nebula's self-absorption frequency.