NS-NS Merger (Mag. Braking) - Revision history

Jake Gordin: /* Observational Constraints */

2018-10-11T11:27:06Z

Observational Constraints

← Older revision		Revision as of 07:27, 11 October 2018
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	== Observational Constraints ==		== Observational Constraints ==

			--

Sulona: /* Model Description */

2018-10-11T10:57:11Z

Model Description

← Older revision		Revision as of 06:57, 11 October 2018
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	== Model Description ==		== Model Description ==
	~~consider~~ the merging of two differentially rotating NSs into a uniformly rotating hypermassive NS. Upon coalescence, the merger spins down and magnetic braking generates coherent radiation. Since the merger rate of NSs is consistent with the expected FRB rate, this model implies that a large fraction of NS mergers must produce FRBs. Significant mass ejections are likely to occur during the merger process, which render FRBs unable to penetrate the ejecta. There is a 1 ms time frame after the maximum rotation speed of the merger is reached and before the release of dynamical ejecta, during which the transmission of a single FRB is possible.
			Consider the merging of two differentially rotating NSs into a uniformly rotating hypermassive NS. Upon coalescence, the merger spins down and magnetic braking generates coherent radiation. Since the merger rate of NSs is consistent with the expected FRB rate, this model implies that a large fraction of NS mergers must produce FRBs. Significant mass ejections are likely to occur during the merger process, which render FRBs unable to penetrate the ejecta. There is a 1 ms time frame after the maximum rotation speed of the merger is reached and before the release of dynamical ejecta, during which the transmission of a single FRB is possible.

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

Emma Platts at 15:00, 26 September 2018

2018-09-26T15:00:30Z

← Older revision		Revision as of 11:00, 26 September 2018
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	\|Type = Single		\|Type = Single
	\|EnergyMechanism = Mag. braking		\|EnergyMechanism = Mag. braking
	\|EmissionMechanism = ~~Curv.~~		\|EmissionMechanism = --
	\|LFRadioCounterpart = Yes		\|LFRadioCounterpart = Yes
	\|HFRadioCounterpart = Yes		\|HFRadioCounterpart = Yes

Emma Platts at 14:12, 26 September 2018

2018-09-26T14:12:05Z

← Older revision		Revision as of 10:12, 26 September 2018
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	== Model Description ==		== Model Description ==
	consider the merging of two ~~di�fferentially~~ rotating NSs into a uniformly rotating hypermassive NS. Upon coalescence, the merger spins down and magnetic braking generates coherent radiation. Since the merger rate of NSs is consistent with the expected FRB rate, this model implies that a large fraction of NS mergers must produce FRBs. ~~Signi�ficant~~ mass ejections are likely to occur during the merger process, which render FRBs unable to penetrate the ejecta. There is a 1 ms time frame after the maximum rotation speed of the merger is reached and before the release of dynamical ejecta, during which the transmission of a single FRB is possible.		consider the merging of two differentially rotating NSs into a uniformly rotating hypermassive NS. Upon coalescence, the merger spins down and magnetic braking generates coherent radiation. Since the merger rate of NSs is consistent with the expected FRB rate, this model implies that a large fraction of NS mergers must produce FRBs. Significant mass ejections are likely to occur during the merger process, which render FRBs unable to penetrate the ejecta. There is a 1 ms time frame after the maximum rotation speed of the merger is reached and before the release of dynamical ejecta, during which the transmission of a single FRB is possible.

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

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

2018-09-26T14:11:41Z

Created page with "   {{FRBTableTemplate |Category = Merger |Pr..."

New page

{{FRBTableTemplate
|Category = Merger
|Progenitor = NS-NS
|Type = Single
|EnergyMechanism = Mag. braking
|EmissionMechanism = Curv.
|LFRadioCounterpart = Yes
|HFRadioCounterpart = Yes
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = Kilonova
|XrayCounterpart = Afterglow
|GammarayCounterpart = sGRB <br/> if jet aligned
|GWCounterpart = Yes
|NeutrinoCounterpart = --
|References = http://adsabs.harvard.edu/abs/2013PASJ...65L..12T
|Comments =
}}

== Model Description ==
consider the merging of two di�fferentially rotating NSs into a uniformly rotating hypermassive NS. Upon coalescence, the merger spins down and magnetic braking generates coherent radiation. Since the merger rate of NSs is consistent with the expected FRB rate, this model implies that a large fraction of NS mergers must produce FRBs. Signi�ficant mass ejections are likely to occur during the merger process, which render FRBs unable to penetrate the ejecta. There is a 1 ms time frame after the maximum rotation speed of the merger is reached and before the release of dynamical ejecta, during which the transmission of a single FRB is possible.

== Observational Constraints ==