WD-WD Merger - Revision history

Apw at 11:26, 9 October 2018

2018-10-09T11:26:42Z

← Older revision		Revision as of 07:26, 9 October 2018
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	== Observational Constraints ==		== Observational Constraints ==
	The event rate of such a scenario is consistent with that predicted for FRBs~~. Whether FRBs can penetrate SN ejecta has, however, been called into question~~.		The event rate of such a scenario is consistent with that predicted for FRBs.

Apw: /* Observational Constraints */

2018-10-09T11:25:46Z

Observational Constraints

← Older revision		Revision as of 07:25, 9 October 2018
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	== Observational Constraints ==		== Observational Constraints ==
	The event rate of such a scenario is consistent with that predicted for FRBs.		The event rate of such a scenario is consistent with that predicted for FRBs. Whether FRBs can penetrate SN ejecta has, however, been called into question.

Apw: /* Model Description */

2018-10-09T11:24:41Z

Model Description

← Older revision		Revision as of 07:24, 9 October 2018
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	== Model Description ==		== Model Description ==
	~~--this needs to be finished--~~
	It has been proposed that FRBs may form when a doubly-degenerate binary WD merger forms a rapidly rotating, magnetized, massive WD. The rapid rotation of the WD merger transports, via convection, inner magnetic fields to the polar regions, which greatly enhances the magnetic field strength. In the polar regions, where the magnetic fields are twisted by differential rotation or magnetic instabilities, reconnection is triggered, and electron bunches are injected into the polar region in a timescale comparable with FRBs. The electrons are accelerated to relativistic speeds along magnetic field lines, creating curvature radiation. WDs transfer angular momentum into the surrounding debris disk, rapidly reducing their rotation speed and hampering multiple FRB events.		It has been proposed that FRBs may form when a doubly-degenerate binary WD merger forms a rapidly rotating, magnetized, massive WD. The rapid rotation of the WD merger transports, via convection, inner magnetic fields to the polar regions, which greatly enhances the magnetic field strength. In the polar regions, where the magnetic fields are twisted by differential rotation or magnetic instabilities, reconnection is triggered, and electron bunches are injected into the polar region in a timescale comparable with FRBs. The electrons are accelerated to relativistic speeds along magnetic field lines, creating curvature radiation. WDs transfer angular momentum into the surrounding debris disk, rapidly reducing their rotation speed and hampering multiple FRB events.

	== Observational Constraints ==		== Observational Constraints ==
	The event rate of such a scenario is consistent with that predicted for FRBs.		The event rate of such a scenario is consistent with that predicted for FRBs.

Apw at 11:24, 9 October 2018

2018-10-09T11:24:07Z

← Older revision		Revision as of 07:24, 9 October 2018
Line 25:		Line 25:
	--this needs to be finished--		--this needs to be finished--
	It has been proposed that FRBs may form when a doubly-degenerate binary WD merger forms a rapidly rotating, magnetized, massive WD. The rapid rotation of the WD merger transports, via convection, inner magnetic fields to the polar regions, which greatly enhances the magnetic field strength. In the polar regions, where the magnetic fields are twisted by differential rotation or magnetic instabilities, reconnection is triggered, and electron bunches are injected into the polar region in a timescale comparable with FRBs. The electrons are accelerated to relativistic speeds along magnetic field lines, creating curvature radiation. WDs transfer angular momentum into the surrounding debris disk, rapidly reducing their rotation speed and hampering multiple FRB events.		It has been proposed that FRBs may form when a doubly-degenerate binary WD merger forms a rapidly rotating, magnetized, massive WD. The rapid rotation of the WD merger transports, via convection, inner magnetic fields to the polar regions, which greatly enhances the magnetic field strength. In the polar regions, where the magnetic fields are twisted by differential rotation or magnetic instabilities, reconnection is triggered, and electron bunches are injected into the polar region in a timescale comparable with FRBs. The electrons are accelerated to relativistic speeds along magnetic field lines, creating curvature radiation. WDs transfer angular momentum into the surrounding debris disk, rapidly reducing their rotation speed and hampering multiple FRB events.

			== Observational Constraints ==
			The event rate of such a scenario is consistent with that predicted for FRBs.

Apw: /* Model Description */

2018-10-09T11:23:16Z

Model Description

← Older revision		Revision as of 07:23, 9 October 2018
Line 24:		Line 24:
	== Model Description ==		== Model Description ==
	--this needs to be finished--		--this needs to be finished--
	It has been proposed that FRBs may form when a doubly-degenerate binary WD merger forms a rapidly rotating, magnetized, massive WD. ~~The event rate of such a scenario is consistent with that predicted for FRBs.~~ The rapid rotation of the WD merger transports, via convection, inner magnetic fields to the polar regions, which greatly enhances the magnetic field strength~~. The corresponding energy budget has been shown to be sufficient for FRB production~~. In the polar regions, where the magnetic fields are twisted by differential rotation or magnetic instabilities, reconnection is triggered, and electron bunches are injected into the polar region in a timescale comparable with FRBs. The electrons are accelerated to relativistic speeds along magnetic field lines, creating curvature radiation. WDs transfer angular momentum into the surrounding debris disk, rapidly reducing their rotation speed and hampering multiple FRB events. ~~The FRBs are predicted to have~~		It has been proposed that FRBs may form when a doubly-degenerate binary WD merger forms a rapidly rotating, magnetized, massive WD. The rapid rotation of the WD merger transports, via convection, inner magnetic fields to the polar regions, which greatly enhances the magnetic field strength. In the polar regions, where the magnetic fields are twisted by differential rotation or magnetic instabilities, reconnection is triggered, and electron bunches are injected into the polar region in a timescale comparable with FRBs. The electrons are accelerated to relativistic speeds along magnetic field lines, creating curvature radiation. WDs transfer angular momentum into the surrounding debris disk, rapidly reducing their rotation speed and hampering multiple FRB events.

Emma Platts at 11:25, 26 September 2018

2018-09-26T11:25:31Z

← Older revision		Revision as of 07:25, 26 September 2018
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	{{FRBTableTemplate		{{FRBTableTemplate
	\|Category = Merger		\|Category = Merger
	\|Progenitor = WD-WD ~~Coalescence~~		\|Progenitor = WD-WD
	\|Type = Single		\|Type = Single
	\|EnergyMechanism = Mag. reconnection		\|EnergyMechanism = Mag. reconnection

Emma Platts at 11:24, 26 September 2018

2018-09-26T11:24:14Z

← Older revision		Revision as of 07:24, 26 September 2018
Line 5:		Line 5:
	{{FRBTableTemplate		{{FRBTableTemplate
	\|Category = Merger		\|Category = Merger
	\|Progenitor = WD-WD		\|Progenitor = WD-WD Coalescence
	\|Type = Single		\|Type = Single
	\|EnergyMechanism = Mag. reconnection		\|EnergyMechanism = Mag. reconnection
Line 23:		Line 23:

	== Model Description ==		== Model Description ==
			--this needs to be finished--
	It has been proposed that FRBs may form when a doubly-degenerate binary WD merger forms a rapidly rotating, magnetized, massive WD. The event rate of such a scenario is consistent with that predicted for FRBs. The rapid rotation of the WD merger transports, via convection, inner magnetic fields to the polar regions, which greatly enhances the magnetic field strength. The corresponding energy budget has been shown to be sufficient for FRB production. In the polar regions, where the magnetic fields are twisted by differential rotation or magnetic instabilities, reconnection is triggered, and electron bunches are injected into the polar region in a timescale comparable with FRBs. The electrons are accelerated to relativistic speeds along magnetic field lines, creating curvature radiation. WDs transfer angular momentum into the surrounding debris disk, rapidly reducing their rotation speed and hampering multiple FRB events. The FRBs are predicted to have		It has been proposed that FRBs may form when a doubly-degenerate binary WD merger forms a rapidly rotating, magnetized, massive WD. The event rate of such a scenario is consistent with that predicted for FRBs. The rapid rotation of the WD merger transports, via convection, inner magnetic fields to the polar regions, which greatly enhances the magnetic field strength. The corresponding energy budget has been shown to be sufficient for FRB production. In the polar regions, where the magnetic fields are twisted by differential rotation or magnetic instabilities, reconnection is triggered, and electron bunches are injected into the polar region in a timescale comparable with FRBs. The electrons are accelerated to relativistic speeds along magnetic field lines, creating curvature radiation. WDs transfer angular momentum into the surrounding debris disk, rapidly reducing their rotation speed and hampering multiple FRB events. The FRBs are predicted to have

Emma Platts at 08:13, 26 September 2018

2018-09-26T08:13:04Z

← Older revision		Revision as of 04:13, 26 September 2018
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	\|MicrowaveCounterpart = --		\|MicrowaveCounterpart = --
	\|THzCounterpart = --		\|THzCounterpart = --
	\|OIRCounterpart = ~~supernova~~		\|OIRCounterpart = Supernova
	\|XrayCounterpart = ~~afterglow~~		\|XrayCounterpart = Afterglow
	\|GammarayCounterpart = --		\|GammarayCounterpart = --
	\|GWCounterpart = --		\|GWCounterpart = --
Line 23:		Line 23:

	== Model Description ==		== Model Description ==
	It has been proposed that FRBs may form when a doubly-degenerate binary WD merger forms a rapidly rotating, magnetized, massive WD. The event rate of such a scenario is consistent with that predicted for FRBs. The rapid rotation of the WD merger transports, via convection, inner magnetic fields to the polar regions, which greatly enhances the magnetic field strength. The corresponding energy budget has been shown to be sufficient for FRB production. In the polar regions, where the magnetic fields are twisted by differential rotation or magnetic instabilities, reconnection is triggered, and electron bunches are injected into the polar region in a timescale comparable with FRBs. The electrons are accelerated to relativistic speeds along magnetic field lines, creating curvature radiation. WDs transfer angular momentum into the surrounding debris disk, rapidly reducing their rotation speed and hampering multiple FRB events. The FRBs are predicted to have ~~one of two possible counter parts: X-ray emission, or a Type Ia supernova (SN) formed upon the collapse of the massive WD.~~		It has been proposed that FRBs may form when a doubly-degenerate binary WD merger forms a rapidly rotating, magnetized, massive WD. The event rate of such a scenario is consistent with that predicted for FRBs. The rapid rotation of the WD merger transports, via convection, inner magnetic fields to the polar regions, which greatly enhances the magnetic field strength. The corresponding energy budget has been shown to be sufficient for FRB production. In the polar regions, where the magnetic fields are twisted by differential rotation or magnetic instabilities, reconnection is triggered, and electron bunches are injected into the polar region in a timescale comparable with FRBs. The electrons are accelerated to relativistic speeds along magnetic field lines, creating curvature radiation. WDs transfer angular momentum into the surrounding debris disk, rapidly reducing their rotation speed and hampering multiple FRB events. The FRBs are predicted to have

	~~== Observational Constraints ==~~

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

2018-09-26T03:50:01Z

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

New page

{{FRBTableTemplate
|Category = Merger
|Progenitor = WD-WD
|Type = Single
|EnergyMechanism = Mag. reconnection
|EmissionMechanism = Curv.
|LFRadioCounterpart = Yes
|HFRadioCounterpart = --
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = supernova
|XrayCounterpart = afterglow
|GammarayCounterpart = --
|GWCounterpart = --
|NeutrinoCounterpart = --
|References = http://adsabs.harvard.edu/abs/2013ApJ...776L..39K
|Comments = --
}}

== Model Description ==
It has been proposed that FRBs may form when a doubly-degenerate binary WD merger forms a rapidly rotating, magnetized, massive WD. The event rate of such a scenario is consistent with that predicted for FRBs. The rapid rotation of the WD merger transports, via convection, inner magnetic fields to the polar regions, which greatly enhances the magnetic field strength. The corresponding energy budget has been shown to be sufficient for FRB production. In the polar regions, where the magnetic fields are twisted by differential rotation or magnetic instabilities, reconnection is triggered, and electron bunches are injected into the polar region in a timescale comparable with FRBs. The electrons are accelerated to relativistic speeds along magnetic field lines, creating curvature radiation. WDs transfer angular momentum into the surrounding debris disk, rapidly reducing their rotation speed and hampering multiple FRB events. The FRBs are predicted to have one of two possible counter parts: X-ray emission, or a Type Ia supernova (SN) formed upon the collapse of the massive WD.

== Observational Constraints ==