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

Apw: /* Model Description */

2018-10-09T10:36:41Z

Model Description

← Older revision		Revision as of 06:36, 9 October 2018
Line 24:		Line 24:
	== Model Description ==		== Model Description ==

	This is an FRB model where the merger of two neutron stars would lead to the generation of an isotropic radio pulse. As the NSs approach each other during the final stages of their inspiral, a toroidal magnetic field is induced around the star’s individual magnetic field lines. The toroidal field strength eventually builds up to rival the poloidal field of the NS magnetospheres, resulting in magnetic reconnection. After reconnection, the toroidal magnetic field becomes weak again and the process can repeat as the NSs continue to spiral inwards. If emission occurs for two orbital periods, a double peaked FRB could be observed~~, as in FRB 120012~~. In this theory, the merger product is presumed to be a rapidly spinning BH.		This is an FRB model where the merger of two neutron stars would lead to the generation of an isotropic radio pulse. As the NSs approach each other during the final stages of their inspiral, a toroidal magnetic field is induced around the star’s individual magnetic field lines. The toroidal field strength eventually builds up to rival the poloidal field of the NS magnetospheres, resulting in magnetic reconnection. After reconnection, the toroidal magnetic field becomes weak again and the process can repeat as the NSs continue to spiral inwards. If emission occurs for two orbital periods, a double peaked FRB could be observed. In this theory, the merger product is presumed to be a rapidly spinning BH.

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

	In general this model would predict that FRBs arise from old stellar populations where NS-NS binary systems have had time to form and evolve into compact orbits.		In general this model would predict that FRBs arise from old stellar populations where NS-NS binary systems have had time to form and evolve into compact orbits.

Apw: /* Model Description */

2018-10-09T10:23:11Z

Model Description

← Older revision		Revision as of 06:23, 9 October 2018
Line 24:		Line 24:
	== Model Description ==		== Model Description ==

	This is an FRB model where the merger of two neutron stars would lead to the generation of an isotropic radio pulse.		This is an FRB model where the merger of two neutron stars would lead to the generation of an isotropic radio pulse. As the NSs approach each other during the final stages of their inspiral, a toroidal magnetic field is induced around the star’s individual magnetic field lines. The toroidal field strength eventually builds up to rival the poloidal field of the NS magnetospheres, resulting in magnetic reconnection. After reconnection, the toroidal magnetic field becomes weak again and the process can repeat as the NSs continue to spiral inwards. If emission occurs for two orbital periods, a double peaked FRB could be observed, as in FRB 120012. In this theory, the merger product is presumed to be a rapidly spinning BH.

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

	In general this model would predict that FRBs arise from old stellar populations where NS-NS binary systems have had time to form and evolve into compact orbits.		In general this model would predict that FRBs arise from old stellar populations where NS-NS binary systems have had time to form and evolve into compact orbits.

Emma Platts at 14:59, 26 September 2018

2018-09-26T14:59:54Z

← Older revision		Revision as of 10:59, 26 September 2018
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	\|GammarayCounterpart = sGRB <br/> if jet aligned		\|GammarayCounterpart = sGRB <br/> if jet aligned
	\|GWCounterpart = Yes		\|GWCounterpart = Yes
	\|NeutrinoCounterpart =		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2016ApJ...822L...7W		\|References = http://adsabs.harvard.edu/abs/2016ApJ...822L...7W
	\|Comments = None		\|Comments = None

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

2018-09-26T14:16:01Z

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

New page

{{FRBTableTemplate
|Category = Merger
|Progenitor = NS-NS
|Type = Both
|EnergyMechanism = Mag. reconnection
|EmissionMechanism = Curv.
|LFRadioCounterpart = Yes (excl. self absorption)
|HFRadioCounterpart = Yes
|MicrowaveCounterpart = ?
|THzCounterpart = ?
|OIRCounterpart = Kilonova
|XrayCounterpart = Afterglow
|GammarayCounterpart = sGRB <br/> if jet aligned
|GWCounterpart = Yes
|NeutrinoCounterpart =
|References = http://adsabs.harvard.edu/abs/2016ApJ...822L...7W
|Comments = None
}}

== Model Description ==

This is an FRB model where the merger of two neutron stars would lead to the generation of an isotropic radio pulse.

== Observational Constraints ==

In general this model would predict that FRBs arise from old stellar populations where NS-NS binary systems have had time to form and evolve into compact orbits.