Magnetars with Low Magnetospheric Twist - Revision history

Emma Platts at 07:43, 20 January 2020

2020-01-20T07:43:28Z

← Older revision		Revision as of 03:43, 20 January 2020
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	\|GWCounterpart = ---		\|GWCounterpart = ---
	\|NeutrinoCounterpart = ---		\|NeutrinoCounterpart = ---
	\|References = https://arxiv.org/pdf/1904.12036.pdf		\|References = https://arxiv.org/pdf/1904.12036.pdf, https://arxiv.org/abs/1910.06979
	\|Comments = Unlikely to form in Galactic magnetars.		\|Comments = Unlikely to form in Galactic magnetars.
	}}		}}

Emma Platts at 08:25, 8 January 2020

2020-01-08T08:25:22Z

← Older revision		Revision as of 04:25, 8 January 2020
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	\|Type = Repeat		\|Type = Repeat
	\|EnergyMechanism = Mag. reconnection		\|EnergyMechanism = Mag. reconnection
	\|EmissionMechanism = ~~Curv.~~		\|EmissionMechanism = Pulsar-like
	\|LFRadioCounterpart = Yes		\|LFRadioCounterpart = Yes
	\|HFRadioCounterpart = ---		\|HFRadioCounterpart = ---

Emma Platts at 19:04, 5 September 2019

2019-09-05T19:04:00Z

← Older revision		Revision as of 15:04, 5 September 2019
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	\|EnergyMechanism = Mag. reconnection		\|EnergyMechanism = Mag. reconnection
	\|EmissionMechanism = Curv.		\|EmissionMechanism = Curv.
	\|LFRadioCounterpart = Yes ~~<br/>(excl. self absorption)~~		\|LFRadioCounterpart = Yes
	\|HFRadioCounterpart = ~~Yes~~		\|HFRadioCounterpart = ---
	\|MicrowaveCounterpart = Maybe		\|MicrowaveCounterpart = Maybe
	\|THzCounterpart = Maybe		\|THzCounterpart = Maybe
	\|OIRCounterpart = No		\|OIRCounterpart = Maybe
	\|XrayCounterpart = ~~Afterglow~~		\|XrayCounterpart = Maybe
	\|GammarayCounterpart = ~~Yes <br/> if jet aligned~~		\|GammarayCounterpart = Unlikely detectable
	\|GWCounterpart = ~~Yes~~		\|GWCounterpart = ---
	\|NeutrinoCounterpart = ---		\|NeutrinoCounterpart = ---
	\|References = https://arxiv.org/pdf/1904.12036.pdf		\|References = https://arxiv.org/pdf/1904.12036.pdf
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	== Model Description ==		== Model Description ==
	FRBs may be ~~the result of short bursts~~ created in the closed field line regions of magnetar magnetospheres. Crustal slippage on the surface of the magnetar causes magnetic reconnection and thus particle acceleration, producing coherent emission. To allow emission to escape, the magnetars must have a low-density plasma in the closed field line regions, and hence must have low magnetospheric twist.		FRBs may be created in the closed field line regions of magnetar magnetospheres. Crustal slippage on the surface of the magnetar causes magnetic reconnection and thus particle acceleration, producing coherent emission. To allow emission to escape, the magnetars must have a low-density plasma in the closed field line regions, and hence must have low magnetospheric twist.

	== Observational Constraints ==		== Observational Constraints ==
	Unlikely to form in Galactic magnetars, which have a relatively high magnetospheric twist. Signals above a few MeV are expected to be suppressed by photon splitting and magnetic pair production in the magnetosphere.		Unlikely to form in Galactic magnetars, which have a relatively high magnetospheric twist. Signals above a few MeV are expected to be suppressed by photon splitting and magnetic pair production in the magnetosphere.

Emma Platts at 18:42, 5 September 2019

2019-09-05T18:42:43Z

← Older revision		Revision as of 14:42, 5 September 2019
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	\|GammarayCounterpart = Yes <br/> if jet aligned		\|GammarayCounterpart = Yes <br/> if jet aligned
	\|GWCounterpart = Yes		\|GWCounterpart = Yes
	\|NeutrinoCounterpart = ~~Not detectable~~		\|NeutrinoCounterpart = ---
	\|References = ~~http~~://~~adsabs~~.~~harvard.edu/abs/2018arXiv180804822P, http:~~//~~adsabs~~.~~harvard~~.~~edu/abs/2018arXiv180804822P~~		\|References = https://arxiv.org/pdf/1904.12036.pdf
	\|Comments = ~~None~~		\|Comments = Unlikely to form in Galactic magnetars.
	}}		}}

	== Model Description ==		== Model Description ==
	FRBs may be the result of short bursts created in the closed field line regions of magnetar magnetospheres ~~(as opposed to near the caps as in pulses)~~. Crustal slippage on the surface of the magnetar causes magnetic reconnection and thus particle acceleration, producing coherent emission.		FRBs may be the result of short bursts created in the closed field line regions of magnetar magnetospheres. Crustal slippage on the surface of the magnetar causes magnetic reconnection and thus particle acceleration, producing coherent emission. To allow emission to escape, the magnetars must have a low-density plasma in the closed field line regions, and hence must have low magnetospheric twist.

	== Observational Constraints ==		== Observational Constraints ==
			Unlikely to form in Galactic magnetars, which have a relatively high magnetospheric twist. Signals above a few MeV are expected to be suppressed by photon splitting and magnetic pair production in the magnetosphere.

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

2019-09-05T18:13:12Z

Created page with "   {{FRBTableTemplate |Category = Other |Pro..."

New page

{{FRBTableTemplate
|Category = Other
|Progenitor = Magnetars with Low Magnetospheric Twist
|Type = Repeat
|EnergyMechanism = Mag. reconnection
|EmissionMechanism = Curv.
|LFRadioCounterpart = Yes <br/>(excl. self absorption)
|HFRadioCounterpart = Yes
|MicrowaveCounterpart = Maybe
|THzCounterpart = Maybe
|OIRCounterpart = No
|XrayCounterpart = Afterglow
|GammarayCounterpart = Yes <br/> if jet aligned
|GWCounterpart = Yes
|NeutrinoCounterpart = Not detectable
|References = http://adsabs.harvard.edu/abs/2018arXiv180804822P, http://adsabs.harvard.edu/abs/2018arXiv180804822P
|Comments = None
}}

== Model Description ==
FRBs may be the result of short bursts created in the closed field line regions of magnetar magnetospheres (as opposed to near the caps as in pulses). Crustal slippage on the surface of the magnetar causes magnetic reconnection and thus particle acceleration, producing coherent emission.

== Observational Constraints ==