Pulsar Wind Bubble - Revision history

Emma Platts at 09:52, 15 October 2018

2018-10-15T09:52:53Z

← Older revision		Revision as of 05:52, 15 October 2018
Line 18:		Line 18:
	\|GWCounterpart = --		\|GWCounterpart = --
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = [http://adsabs.harvard.edu/abs/2017MNRAS.467.3542M]		\|References = http://adsabs.harvard.edu/abs/2017MNRAS.467.3542M
	\|Comments = None		\|Comments = None
	}}		}}

Emma Platts at 09:51, 15 October 2018

2018-10-15T09:51:06Z

← Older revision		Revision as of 05:51, 15 October 2018
Line 18:		Line 18:
	\|GWCounterpart = --		\|GWCounterpart = --
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2017MNRAS.467.3542M		\|References = [http://adsabs.harvard.edu/abs/2017MNRAS.467.3542M]
	\|Comments = None		\|Comments = None
	}}		}}

Emma Platts at 09:50, 12 October 2018

2018-10-12T09:50:46Z

← Older revision		Revision as of 05:50, 12 October 2018
Line 19:		Line 19:
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2017MNRAS.467.3542M		\|References = http://adsabs.harvard.edu/abs/2017MNRAS.467.3542M
	\|Comments = ~~Emission from the PWN as it expands outwards might be detected in the NS scenario. A SN a few years prior to the FRB may be observed for either body.~~		\|Comments = None
	}}		}}

	== Model Description ==		== Model Description ==
	Consider a pulsar (NS or magnetic WD, hereafter MWD) within a nebula. The dissipation of spin energy drives a wind of relativistic electron-positron plasma--a pulsar wind nebula (PWN)--observable as a shell around the NS. Where the plasma wind ceases is called the termination shock. Here the plasma decelerates to sub-relativistic speeds and forms a wind bubble around the pulsar. A subsequent outburst, possibly triggered by pulsar spin-down or by magnetic dissipation in the magnetosphere, will rapidly decelerate when it impacts the PWN, triggering a GRB. Energy that is not radiated away by the explosion itself travels outwards at a relativistic speed, causing a highly relativistic shock wave to propagates forward into space. Synchrotron emission is generated, however the coherence mechanism to generate FRBs at this point is unknown. A synchrotron maser might result from the coherently reflected particles in the shock front, but for NSs and magnetic MWDs the frequency is likely too low to be consistent with FRBs. A reverse shock wave may give rise to afterglow, however both this afterglow and the GRB formed at the shock front are not expected to be observable.		Consider a pulsar (NS or magnetic WD, hereafter MWD) within a nebula. The dissipation of spin energy drives a wind of relativistic electron-positron plasma-a pulsar wind nebula (PWN)-observable as a shell around the NS. Where the plasma wind ceases is called the termination shock. Here the plasma decelerates to sub-relativistic speeds and forms a wind bubble around the pulsar. A subsequent outburst, possibly triggered by pulsar spin-down or by magnetic dissipation in the magnetosphere, will rapidly decelerate when it impacts the PWN, triggering a GRB. Energy that is not radiated away by the explosion itself travels outwards at a relativistic speed, causing a highly relativistic shock wave to propagates forward into space. Synchrotron emission is generated, however the coherence mechanism to generate FRBs at this point is unknown. A synchrotron maser might result from the coherently reflected particles in the shock front, but for NSs and magnetic MWDs the frequency is likely too low to be consistent with FRBs. A reverse shock wave may give rise to afterglow, however both this afterglow and the GRB formed at the shock front are not expected to be observable.

	== Observational Constraints ==		== Observational Constraints ==
			Emission from the PWN as it expands outwards might be detected in the NS scenario. A SN a few years prior to the FRB may be observed for either body.
	--

Emma Platts at 09:48, 12 October 2018

2018-10-12T09:48:21Z

← Older revision		Revision as of 05:48, 12 October 2018
Line 14:		Line 14:
	\|THzCounterpart = --		\|THzCounterpart = --
	\|OIRCounterpart = --		\|OIRCounterpart = --
	\|XrayCounterpart = ~~ULXs~~		\|XrayCounterpart = Yes
	\|GammarayCounterpart = --		\|GammarayCounterpart = --
	\|GWCounterpart = --		\|GWCounterpart = --

Jake Gordin: /* Observational Constraints */

2018-10-11T11:28:18Z

Observational Constraints

← Older revision		Revision as of 07:28, 11 October 2018
Line 26:		Line 26:

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

			--

Emma Platts at 14:50, 27 September 2018

2018-09-27T14:50:49Z

← Older revision		Revision as of 10:50, 27 September 2018
Line 7:		Line 7:
	\|Progenitor = Pulsar Wind Bubble (NS and MWD)		\|Progenitor = Pulsar Wind Bubble (NS and MWD)
	\|Type = Single		\|Type = Single
	\|EnergyMechanism = ~~Open Question~~		\|EnergyMechanism = --
	\|EmissionMechanism = Synch.		\|EmissionMechanism = Synch.
	\|LFRadioCounterpart = Yes		\|LFRadioCounterpart = Yes

Emma Platts at 12:04, 27 September 2018

2018-09-27T12:04:01Z

← Older revision		Revision as of 08:04, 27 September 2018
Line 18:		Line 18:
	\|GWCounterpart = --		\|GWCounterpart = --
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/~~2018arXiv180804822P, http://adsabs~~.~~harvard~~.~~edu/abs/2018arXiv180804822P~~		\|References = http://adsabs.harvard.edu/abs/2017MNRAS.467.3542M
	\|Comments = Emission from the PWN as it expands outwards might be detected in the NS scenario. A SN a few years prior to the FRB may be observed for either body.		\|Comments = Emission from the PWN as it expands outwards might be detected in the NS scenario. A SN a few years prior to the FRB may be observed for either body.
	}}		}}

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

2018-09-27T11:53:41Z

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

New page

{{FRBTableTemplate
|Category = SNR (Pulsars)
|Progenitor = Pulsar Wind Bubble (NS and MWD)
|Type = Single
|EnergyMechanism = Open Question
|EmissionMechanism = Synch.
|LFRadioCounterpart = Yes
|HFRadioCounterpart = --
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = --
|XrayCounterpart = ULXs
|GammarayCounterpart = --
|GWCounterpart = --
|NeutrinoCounterpart = --
|References = http://adsabs.harvard.edu/abs/2018arXiv180804822P, http://adsabs.harvard.edu/abs/2018arXiv180804822P
|Comments = Emission from the PWN as it expands outwards might be detected in the NS scenario. A SN a few years prior to the FRB may be observed for either body.
}}

== Model Description ==
Consider a pulsar (NS or magnetic WD, hereafter MWD) within a nebula. The dissipation of spin energy drives a wind of relativistic electron-positron plasma--a pulsar wind nebula (PWN)--observable as a shell around the NS. Where the plasma wind ceases is called the termination shock. Here the plasma decelerates to sub-relativistic speeds and forms a wind bubble around the pulsar. A subsequent outburst, possibly triggered by pulsar spin-down or by magnetic dissipation in the magnetosphere, will rapidly decelerate when it impacts the PWN, triggering a GRB. Energy that is not radiated away by the explosion itself travels outwards at a relativistic speed, causing a highly relativistic shock wave to propagates forward into space. Synchrotron emission is generated, however the coherence mechanism to generate FRBs at this point is unknown. A synchrotron maser might result from the coherently reflected particles in the shock front, but for NSs and magnetic MWDs the frequency is likely too low to be consistent with FRBs. A reverse shock wave may give rise to afterglow, however both this afterglow and the GRB formed at the shock front are not expected to be observable.

== Observational Constraints ==