NS Combing - Revision history

Sulona: /* Observational Constraints */

2018-10-11T11:07:57Z

Observational Constraints

← Older revision		Revision as of 07:07, 11 October 2018
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	== Observational Constraints ==		== Observational Constraints ==

	~~To be filled in with updated draft~~		N/A

Sulona: /* Model Description */

2018-10-11T11:04:22Z

Model Description

← Older revision		Revision as of 07:04, 11 October 2018
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	== Model Description ==		== Model Description ==

	To be ~~filled in~~ with ~~updated draft~~
			Cosmic combing is the process in which the field lines of a NS's magnetosphere are swept out in a stream by a strong plasma. The effect is caused by ram pressure: the bulk resistance of a fluid acting on an object. When this pressure is greater than the magnetic field pressure, the drag will comb the magnetic field in a different direction, causing reconnection with emission consistent with an FRB . Combing may occur in a variety of situations, such as: a GRB, a SN, an AGN flare, or a stellar flare. As such, it is a difficult theory to test in general, however a specific scenario has been considered: the combing of a pulsar by an accreting SMBH. An FRB would be observable for half of the pulsar's orbital period around the SMBH, implying the signal is periodic. This periodicity would not be perfect - the SMBH wind that initiates FRBs is variable and thus FRB signals are sporadic. The RM should vary with orbital periodicity, but this would be more difficult to confirm given the sporadic FRB emission. Finally, the polarization angle of each burst within an orbital period would vary depending on the phase of the pulsar's orbit, and should be correlated with the varying RM.

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

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

Jake Gordin at 09:42, 11 October 2018

2018-10-11T09:42:59Z

← Older revision		Revision as of 05:42, 11 October 2018
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	\|GWCounterpart = --		\|GWCounterpart = --
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2017ApJ...836L..32Z, ~~https~~://~~arxiv~~.~~org~~/~~pdf~~/1801.05436~~.pdf~~		\|References = http://adsabs.harvard.edu/abs/2017ApJ...836L..32Z, http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1801.05436
	\|Comments = The model can apply to a variety of events, and thus counterparts will depend on the scenario.		\|Comments = The model can apply to a variety of events, and thus counterparts will depend on the scenario.
	}}		}}

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

2018-10-02T14:24:06Z

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

New page

{{FRBTableTemplate
|Category = Other
|Progenitor = NS Combing
|Type = Both
|EnergyMechanism = Various
|EmissionMechanism = Mag. reconnection
|LFRadioCounterpart = Yes
|HFRadioCounterpart = --
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = --
|XrayCounterpart = --
|GammarayCounterpart = --
|GWCounterpart = --
|NeutrinoCounterpart = --
|References = http://adsabs.harvard.edu/abs/2017ApJ...836L..32Z, https://arxiv.org/pdf/1801.05436.pdf
|Comments = The model can apply to a variety of events, and thus counterparts will depend on the scenario.
}}

== Model Description ==

To be filled in with updated draft

== Observational Constraints ==

To be filled in with updated draft