Young Magnetars - Revision history

Emma Platts at 14:23, 6 September 2019

2019-09-06T14:23:33Z

← Older revision		Revision as of 10:23, 6 September 2019
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	\|EnergyMechanism = Maser		\|EnergyMechanism = Maser
	\|EmissionMechanism = Synch.		\|EmissionMechanism = Synch.
	\|LFRadioCounterpart = Yes~~, persistent~~		\|LFRadioCounterpart = Yes
	\|HFRadioCounterpart = ~~Yes, persistent~~		\|HFRadioCounterpart = Afterglow
	\|MicrowaveCounterpart = ~~Maybe~~		\|MicrowaveCounterpart = --
	\|THzCounterpart = ~~Maybe~~		\|THzCounterpart = --
	\|OIRCounterpart = Possible SN		\|OIRCounterpart = Possible SN
	\|XrayCounterpart = Afterglow		\|XrayCounterpart = Afterglow
	\|GammarayCounterpart = ~~SGRB~~		\|GammarayCounterpart = sGRB
	\|GWCounterpart = Yes		\|GWCounterpart = Yes
	\|NeutrinoCounterpart = ~~Not detectable~~		\|NeutrinoCounterpart = --
	\|References = https://arxiv.org/pdf/1907.00016.pdf		\|References = https://arxiv.org/pdf/1907.00016.pdf
	\|Comments = Same mechanisms as flares, but magnetars born in mergers or collapse as opposed in to SLSNe or LGRBs.		\|Comments = Same mechanisms as flares, but magnetars born in mergers or collapse as opposed in to SLSNe or LGRBs.
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	== Observational Constraints ==		== Observational Constraints ==

	~~SGRBs~~ are expected in BNS mergers. The accretion-induced collapse of a WD has yet to be observed but might produce a SN Type Ia-like transient. Persistent synchrotron radio emission may be observable with timescales of months to years from the nebula or on longer timescales when the merger ejecta interacts with the ISM, but is shorter than for the SLSNe/LGRBs. BNS mergers are expected in all galaxy types and may be spatially offset from their birth sites or host galaxies.		sGRBs are expected in BNS mergers. The accretion-induced collapse of a WD has yet to be observed but might produce a SN Type Ia-like transient. Persistent synchrotron radio emission may be observable with timescales of months to years from the nebula or on longer timescales when the merger ejecta interacts with the ISM, but is shorter than for the SLSNe/LGRBs. BNS mergers are expected in all galaxy types and may be spatially offset from their birth sites or host galaxies.

Emma Platts at 14:17, 6 September 2019

2019-09-06T14:17:15Z

← Older revision		Revision as of 10:17, 6 September 2019
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	{{FRBTableTemplate		{{FRBTableTemplate
	\|Category = Merger/Collapse		\|Category = Merger/Collapse
	\|Progenitor = Magnetars Born in ~~NS-NS~~ Mergers and WD Collapse		\|Progenitor = Magnetars Born in BNS Mergers and WD Collapse
	\|Type = Repeat		\|Type = Repeat
	\|EnergyMechanism = Maser		\|EnergyMechanism = Maser
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	\|MicrowaveCounterpart = Maybe		\|MicrowaveCounterpart = Maybe
	\|THzCounterpart = Maybe		\|THzCounterpart = Maybe
	\|OIRCounterpart = No		\|OIRCounterpart = Possible SN
	\|XrayCounterpart = Afterglow		\|XrayCounterpart = Afterglow
	\|GammarayCounterpart = ~~Yes <br/> if jet aligned~~		\|GammarayCounterpart = SGRB
	\|GWCounterpart = Yes		\|GWCounterpart = Yes
	\|NeutrinoCounterpart = Not detectable		\|NeutrinoCounterpart = Not detectable
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	== Model Description ==		== Model Description ==
	~~This model considers~~ FRBs from magnetars born in ~~NS-NS~~ mergers and accretion induced WD collapse. The FRBs themselves are formed by the same mechanism as that of giant flare FRB theories.		The localization of FRB 180924 to the outskirts of a massive early-type host galaxy suggests FRBs may be from magnetars born in binary neutron star (BNS) mergers and accretion induced WD collapse. The FRBs themselves are formed by the same mechanism as that of giant flare FRB theories.

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

	Persistent synchrotron radio emission with timescales of months to years from the nebula or on longer timescales when the merger ejecta interacts with the ISM, but is shorter than for the SLSNe/LGRBs. ~~The accretion-induced collapse of a WD has yet to~~ be ~~observed but might produce a SNIa-like transient~~.		SGRBs are expected in BNS mergers. The accretion-induced collapse of a WD has yet to be observed but might produce a SN Type Ia-like transient. Persistent synchrotron radio emission may be observable with timescales of months to years from the nebula or on longer timescales when the merger ejecta interacts with the ISM, but is shorter than for the SLSNe/LGRBs. BNS mergers are expected in all galaxy types and may be spatially offset from their birth sites or host galaxies.


	== ==		== Consistency with Observations ==

	Using FRB 121102 to calibrate the model, the expected DM, RM and persistent radio emission is consistent with the upper limits of FRB 180924. ~~FRBs from NS-NS magnetars distinct~~ host galaxy and ~~spatial~~ offset distributions ~~than the SLSNe/LGRB channel; we anticipate asimilar host population, although possibly different offset distribution for AIC events~~. It may be more difficult to detect persistent nebular radio emission from known FRB positions than in the SLSN/LGRB case because of high ejecta velocity and low ejecta mass: the emission peaks at early times and the ejecta become transparent to free-free absorption earlier. This is consistent with the non-detection of persistent emission from FRB 180924 and could explain its lower RM.		Using FRB 121102 to calibrate the model, the expected DM, RM and persistent radio emission is consistent with the upper limits of FRB 180924. The host galaxy and offset of FRB 180924 from the center are consistent with distributions of SGRBs and Type Ia SNe. It may be more difficult to detect persistent nebular radio emission from known FRB positions than in the SLSN/LGRB case because of high ejecta velocity and low ejecta mass: the emission peaks at early times and the ejecta become transparent to free-free absorption earlier. This is consistent with the non-detection of persistent emission from FRB 180924 and could explain its lower RM.

Emma Platts at 14:01, 6 September 2019

2019-09-06T14:01:39Z

← Older revision		Revision as of 10:01, 6 September 2019
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	== Observational Constraints ==		== Observational Constraints ==

	Persistent synchrotron radio emission with timescales of months to years from the nebula or on longer timescales when the merger ejecta interacts with the ISM, but is shorter than for the SLSNe/LGRBs.		Persistent synchrotron radio emission with timescales of months to years from the nebula or on longer timescales when the merger ejecta interacts with the ISM, but is shorter than for the SLSNe/LGRBs. The accretion-induced collapse of a WD has yet to be observed but might produce a SNIa-like transient.


	== ==		== ==

	Using FRB 121102 to calibrate the model, the expected DM, RM and persistent radio emission is consistent with the upper limits of FRB 180924. FRBs from NS-NS magnetars distinct host galaxy and spatial offset distributions than the SLSNe/LGRB channel; we anticipate asimilar host population, although possibly different offset distribution for AIC events.		Using FRB 121102 to calibrate the model, the expected DM, RM and persistent radio emission is consistent with the upper limits of FRB 180924. FRBs from NS-NS magnetars distinct host galaxy and spatial offset distributions than the SLSNe/LGRB channel; we anticipate asimilar host population, although possibly different offset distribution for AIC events. It may be more difficult to detect persistent nebular radio emission from known FRB positions than in the SLSN/LGRB case because of high ejecta velocity and low ejecta mass: the emission peaks at early times and the ejecta become transparent to free-free absorption earlier. This is consistent with the non-detection of persistent emission from FRB 180924 and could explain its lower RM.

Emma Platts at 13:47, 6 September 2019

2019-09-06T13:47:12Z

← Older revision		Revision as of 09:47, 6 September 2019
Line 9:		Line 9:
	\|EnergyMechanism = Maser		\|EnergyMechanism = Maser
	\|EmissionMechanism = Synch.		\|EmissionMechanism = Synch.
	\|LFRadioCounterpart = Yes ~~<br/>(excl. self absorption)~~		\|LFRadioCounterpart = Yes, persistent
	\|HFRadioCounterpart = Yes		\|HFRadioCounterpart = Yes, persistent
	\|MicrowaveCounterpart = Maybe		\|MicrowaveCounterpart = Maybe
	\|THzCounterpart = Maybe		\|THzCounterpart = Maybe
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	== Observational Constraints ==		== Observational Constraints ==

	~~FRBs from magnetars born in NS-NS mergers and accretion induced WD collapse will be accompanied by persistent~~ synchrotron radio ~~emissionon~~ timescales of months to years~~, powered by~~ the nebula ~~of relativistic electrons and magnetic fields inflated by the magnetar flares,~~ or on longer timescales ~~through interaction of~~ the merger ejecta with the ~~interstellar medium; this timescale~~ is shorter than for the ~~SLSN~~/~~LGRB channel~~.		Persistent synchrotron radio emission with timescales of months to years from the nebula or on longer timescales when the merger ejecta interacts with the ISM, but is shorter than for the SLSNe/LGRBs.


	~~The~~ DM, RM and persistent radio emission ~~in the model~~ is consistent with		== ==

			Using FRB 121102 to calibrate the model, the expected DM, RM and persistent radio emission is consistent with the upper limits of FRB 180924. FRBs from NS-NS magnetars distinct host galaxy and spatial offset distributions than the SLSNe/LGRB channel; we anticipate asimilar host population, although possibly different offset distribution for AIC events.

Emma Platts at 13:24, 6 September 2019

2019-09-06T13:24:14Z

← Older revision		Revision as of 09:24, 6 September 2019
Line 27:		Line 27:
	== Observational Constraints ==		== Observational Constraints ==

	FRBs from magnetars born in NS-NS mergers and accretion induced WD collapse will be accompanied by persistent synchrotron radio emissionon timescales of months to years, powered by the nebula of relativistic electrons and magnetic fields inflated by the magnetar flares, or on longer timescales through interaction of the merger ejecta with the interstellar medium; this timescale is shorter than for the SLSN/LGRB channel.		FRBs from magnetars born in NS-NS mergers and accretion induced WD collapse will be accompanied by persistent synchrotron radio emissionon timescales of months to years, powered by the nebula of relativistic electrons and magnetic fields inflated by the magnetar flares, or on longer timescales through interaction of the merger ejecta with the interstellar medium; this timescale is shorter than for the SLSN/LGRB channel.


			The DM, RM and persistent radio emission in the model is consistent with

Emma Platts at 13:14, 6 September 2019

2019-09-06T13:14:05Z

← Older revision		Revision as of 09:14, 6 September 2019
Line 23:		Line 23:

	== Model Description ==		== Model Description ==
			This model considers FRBs from magnetars born in NS-NS mergers and accretion induced WD collapse. The FRBs themselves are formed by the same mechanism as that of giant flare FRB theories.
	~~A broader description, observational effects~~ and ~~detailed information~~.
	~~This is an FRB model where~~ the ~~merger~~ of ~~two neutron stars would lead to the generation of an isotropic radio pulse~~.

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

	~~In general this model would predict that~~ FRBs ~~arise~~ from ~~old stellar populations where~~ NS-NS ~~binary systems have had time~~ to ~~form~~ and ~~evolve into compact orbits~~.		FRBs from magnetars born in NS-NS mergers and accretion induced WD collapse will be accompanied by persistent synchrotron radio emissionon timescales of months to years, powered by the nebula of relativistic electrons and magnetic fields inflated by the magnetar flares, or on longer timescales through interaction of the merger ejecta with the interstellar medium; this timescale is shorter than for the SLSN/LGRB channel.

Emma Platts: Created page with " {{FRBTableTemplate |Category = Merger/Col..."

2019-09-06T13:02:06Z

Created page with "   {{FRBTableTemplate |Category = Merger/Col..."

New page

{{FRBTableTemplate
|Category = Merger/Collapse
|Progenitor = Magnetars Born in NS-NS Mergers and WD Collapse
|Type = Repeat
|EnergyMechanism = Maser
|EmissionMechanism = Synch.
|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 = https://arxiv.org/pdf/1907.00016.pdf
|Comments = Same mechanisms as flares, but magnetars born in mergers or collapse as opposed in to SLSNe or LGRBs.
}}

== Model Description ==

A broader description, observational effects and detailed information.
This is an FRB model where the merger of two neutron stars would lead to the generation of an isotropic radio pulse.

== Observational Constraints ==

In general this model would predict that FRBs arise from old stellar populations where NS-NS binary systems have had time to form and evolve into compact orbits.