Giant Pulses - Revision history

Emma Platts at 10:40, 15 October 2018

2018-10-15T10:40:18Z

← Older revision		Revision as of 06:40, 15 October 2018
Line 19:		Line 19:
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2012MNRAS.425L..71K, http://adsabs.harvard.edu/abs/2016MNRAS.457..232C, https://arxiv.org/pdf/1505.05535.pdf		\|References = http://adsabs.harvard.edu/abs/2012MNRAS.425L..71K, http://adsabs.harvard.edu/abs/2016MNRAS.457..232C, https://arxiv.org/pdf/1505.05535.pdf
	\|Comments = ~~None~~		\|Comments = Rapid flux decay expected to be observed within a few years.
	}}		}}

Emma Platts at 09:12, 12 October 2018

2018-10-12T09:12:04Z

← Older revision		Revision as of 05:12, 12 October 2018
Line 19:		Line 19:
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2012MNRAS.425L..71K, http://adsabs.harvard.edu/abs/2016MNRAS.457..232C, https://arxiv.org/pdf/1505.05535.pdf		\|References = http://adsabs.harvard.edu/abs/2012MNRAS.425L..71K, http://adsabs.harvard.edu/abs/2016MNRAS.457..232C, https://arxiv.org/pdf/1505.05535.pdf
	\|Comments = ~~The inferred RMs do not fit well with data.~~		\|Comments = None
	}}		}}

Emma Platts at 14:48, 27 September 2018

2018-09-27T14:48:49Z

← Older revision		Revision as of 10:48, 27 September 2018
Line 7:		Line 7:
	\|Progenitor = Giant Pulses		\|Progenitor = Giant Pulses
	\|Type = Repeat		\|Type = Repeat
	\|EnergyMechanism = ~~Open Question~~		\|EnergyMechanism = --
	\|EmissionMechanism = Synch. <br/> / Curv.		\|EmissionMechanism = Synch. <br/> / Curv.
	\|LFRadioCounterpart = Yes		\|LFRadioCounterpart = Yes

Emma Platts at 11:22, 27 September 2018

2018-09-27T11:22:09Z

← Older revision		Revision as of 07:22, 27 September 2018
Line 7:		Line 7:
	\|Progenitor = Giant Pulses		\|Progenitor = Giant Pulses
	\|Type = Repeat		\|Type = Repeat
	\|EnergyMechanism = ~~Various~~		\|EnergyMechanism = Open Question
	\|EmissionMechanism = Synch. <br/> / Curv.		\|EmissionMechanism = Synch. <br/> / Curv.
	\|LFRadioCounterpart = Yes		\|LFRadioCounterpart = Yes

Emma Platts at 11:19, 27 September 2018

2018-09-27T11:19:35Z

← Older revision		Revision as of 07:19, 27 September 2018
Line 4:		Line 4:
	<!-- This is an example. Change the right hand side of all these assignments -->		<!-- This is an example. Change the right hand side of all these assignments -->
	{{FRBTableTemplate		{{FRBTableTemplate
	\|Category = SNR		\|Category = SNR (Pulsars)
	\|Progenitor = Giant Pulses		\|Progenitor = Giant Pulses
	\|Type = Repeat		\|Type = Repeat

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

2018-09-27T11:19:08Z

Created page with "   {{FRBTableTemplate |Category = SNR |Proge..."

New page

{{FRBTableTemplate
|Category = SNR
|Progenitor = Giant Pulses
|Type = Repeat
|EnergyMechanism = Various
|EmissionMechanism = Synch. <br/> / Curv.
|LFRadioCounterpart = Yes
|HFRadioCounterpart = --
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = --
|XrayCounterpart = --
|GammarayCounterpart = --
|GWCounterpart = --
|NeutrinoCounterpart = --
|References = http://adsabs.harvard.edu/abs/2012MNRAS.425L..71K, http://adsabs.harvard.edu/abs/2016MNRAS.457..232C, https://arxiv.org/pdf/1505.05535.pdf
|Comments = The inferred RMs do not fit well with data.
}}

== Model Description ==

Analogous to models for the Crab pulsar, FRBs of extragalactic origins may be giant pulses of a young pulsar. A specific giant pulse mechanism has been proposed for FRBs, in which a nearly charge-neutral clump of particles (produced by a two-streaming instability or a bunching instability) is accelerated through the pulsar magnetosphere by some reconnection event. The resultant coherent curvature radiation will be emitted for the duration that the clump remains intact. Note, however, that the emission mechanism of giant pulses remains an open question, and that this represents one possibility for FRB formation.

== Observational Constraints ==
FRBs are predicted to be repeating and stochastic. A SN explosion a few years prior to the FRB may be observable. The DM, RM and polarization of FRBs in this scenario are owed to the nebula surrounding the pulsar as opposed to the intergalactic medium. This places FRBs at extragalactic (as opposed to cosmological) distances, and thus relaxes the energy requirements. The spin-down luminosity decreases within a timescale of a few years. The giant pulse model therefore depends on the observation of rapid flux decay in FRBs within a few years.