Wandering Pulsar - Revision history

Sulona: /* Model Description */

2018-10-11T15:58:53Z

Model Description

← Older revision		Revision as of 11:58, 11 October 2018
Line 24:		Line 24:
	== Model Description ==		== Model Description ==

	This model assumes the presence of a steady beam of pulsar emission whose ~~directlion~~ randomly changes. If this beam sweeps across the line of sight of an observer, it may be observable as an FRB. The duration of the FRB depends on the speed at which the beam moves across the sky, and hence a wandering beam mitigates the enormous power and high spin-down requirements of giant pulse and flare models.		This model assumes the presence of a steady beam of pulsar emission whose direction randomly changes. If this beam sweeps across the line of sight of an observer, it may be observable as an FRB. The duration of the FRB depends on the speed at which the beam moves across the sky, and hence a wandering beam mitigates the enormous power and high spin-down requirements of giant pulse and flare models.

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

	This scenario can also consistently explain two pairs of possibly distinct radio bursts detected in FRB 121102. Details about an emission mechanism or possible counterparts are not given.		This scenario can also consistently explain two pairs of possibly distinct radio bursts detected in FRB 121102. Details about an emission mechanism or possible counterparts are not given.

Sulona: /* Model Description */

2018-10-11T15:58:21Z

Model Description

← Older revision		Revision as of 11:58, 11 October 2018
Line 24:		Line 24:
	== Model Description ==		== Model Description ==

	This model assumes the presence of a steady beam of pulsar emission whose ~~directly~~ randomly changes. If this beam sweeps across the line of sight of an observer, it may be observable as an FRB. The duration of the FRB depends on the speed at which the beam moves across the sky, and hence a wandering beam mitigates the enormous power and high spin-down requirements of giant pulse and flare models.		This model assumes the presence of a steady beam of pulsar emission whose directlion randomly changes. If this beam sweeps across the line of sight of an observer, it may be observable as an FRB. The duration of the FRB depends on the speed at which the beam moves across the sky, and hence a wandering beam mitigates the enormous power and high spin-down requirements of giant pulse and flare models.

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

	This scenario can also consistently explain two pairs of possibly distinct radio bursts detected in FRB 121102. Details about an emission mechanism or possible counterparts are not given.		This scenario can also consistently explain two pairs of possibly distinct radio bursts detected in FRB 121102. Details about an emission mechanism or possible counterparts are not given.

Jake Gordin at 10:00, 11 October 2018

2018-10-11T10:00:51Z

← Older revision		Revision as of 06:00, 11 October 2018
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	\|GWCounterpart = --		\|GWCounterpart = --
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = ~~https~~://~~arxiv~~.~~org~~/~~pdf~~/1611.01243~~.pdf~~		\|References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1611.01243
	\|Comments = Any counterparts will be associated with the pulsar, but are not specified.		\|Comments = Any counterparts will be associated with the pulsar, but are not specified.
	}}		}}

Apw: /* Observational Constraints */

2018-10-09T11:12:12Z

Observational Constraints

← Older revision		Revision as of 07:12, 9 October 2018
Line 28:		Line 28:
	== Observational Constraints ==		== Observational Constraints ==

	~~To be filled~~ in ~~with updated draft~~		This scenario can also consistently explain two pairs of possibly distinct radio bursts detected in FRB 121102. Details about an emission mechanism or possible counterparts are not given.

Apw: /* Model Description */

2018-10-09T11:09:42Z

Model Description

← Older revision		Revision as of 07:09, 9 October 2018
Line 24:		Line 24:
	== Model Description ==		== Model Description ==

	To be ~~filled in with updated draft~~		This model assumes the presence of a steady beam of pulsar emission whose directly randomly changes. If this beam sweeps across the line of sight of an observer, it may be observable as an FRB. The duration of the FRB depends on the speed at which the beam moves across the sky, and hence a wandering beam mitigates the enormous power and high spin-down requirements of giant pulse and flare models.

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

	To be filled in with updated draft		To be filled in with updated draft

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

2018-10-02T14:05:18Z

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

New page

{{FRBTableTemplate
|Category = Other
|Progenitor = Wandering Pulsar Beams
|Type = Repeat
|EnergyMechanism = --
|EmissionMechanism = --
|LFRadioCounterpart = Yes
|HFRadioCounterpart = --
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = --
|XrayCounterpart = --
|GammarayCounterpart = --
|GWCounterpart = --
|NeutrinoCounterpart = --
|References = https://arxiv.org/pdf/1611.01243.pdf
|Comments = Any counterparts will be associated with the pulsar, but are not specified.
}}

== Model Description ==

To be filled in with updated draft

== Observational Constraints ==

To be filled in with updated draft