NS-SN Interaction - Revision history

Apw at 12:40, 10 October 2018

2018-10-10T12:40:13Z

← Older revision		Revision as of 08:40, 10 October 2018
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	== Observational Constraints ==		== Observational Constraints ==

	A GRB is expected, but with a low flux that may be difficult to detect. A core-collapse supernova is expected to be coincident with the FRB.		A GRB is expected, but with a low flux that may be difficult to detect. A core-collapse supernova is expected to be coincident with the FRB.

Apw at 09:44, 9 October 2018

2018-10-09T09:44:13Z

← Older revision		Revision as of 05:44, 9 October 2018
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	\|OIRCounterpart = Supernova		\|OIRCounterpart = Supernova
	\|XrayCounterpart = --		\|XrayCounterpart = --
	\|GammarayCounterpart = --		\|GammarayCounterpart = possible GRB (low flux)
	\|GWCounterpart = --		\|GWCounterpart = --
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --

Apw: /* Observational Constraints */

2018-10-09T09:36:13Z

Observational Constraints

← Older revision		Revision as of 05:36, 9 October 2018
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	== Observational Constraints ==		== Observational Constraints ==
	~~A core-collapse supernova is expected to be coincident with the FRB.~~ A GRB is expected ~~in such an event~~, but with a low flux that may be difficult to detect.		A GRB is expected, but with a low flux that may be difficult to detect. A core-collapse supernova is expected to be coincident with the FRB.

Apw: /* Model Description */

2018-10-09T09:35:35Z

Model Description

← Older revision		Revision as of 05:35, 9 October 2018
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	with the magnetosphere of a NS in a binary system. When the shock encounters the NS		with the magnetosphere of a NS in a binary system. When the shock encounters the NS
	magnetosphere, it sweeps out a magnetospheric tail, which triggers reconnection and hence		magnetosphere, it sweeps out a magnetospheric tail, which triggers reconnection and hence
	emission~~. A GRB is expected in such an event, but with a low flux that may be difficult to detect~~.		emission.

	== Observational Constraints ==		== Observational Constraints ==
	A core-collapse supernova is expected to be coincident with the FRB. A GRB is expected in such an event, but with a low flux that may be difficult to detect.		A core-collapse supernova is expected to be coincident with the FRB. A GRB is expected in such an event, but with a low flux that may be difficult to detect.

Apw: /* Observational Constraints */

2018-10-09T09:35:12Z

Observational Constraints

← Older revision		Revision as of 05:35, 9 October 2018
Line 30:		Line 30:

	== Observational Constraints ==		== Observational Constraints ==
	A core-collapse supernova is expected to be coincident with the FRB.		A core-collapse supernova is expected to be coincident with the FRB. A GRB is expected in such an event, but with a low flux that may be difficult to detect.

Apw: /* Model Description */

2018-10-09T09:33:54Z

Model Description

← Older revision		Revision as of 05:33, 9 October 2018
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	with the magnetosphere of a NS in a binary system. When the shock encounters the NS		with the magnetosphere of a NS in a binary system. When the shock encounters the NS
	magnetosphere, it sweeps out a magnetospheric tail, which triggers reconnection and hence		magnetosphere, it sweeps out a magnetospheric tail, which triggers reconnection and hence
	emission. A GRB is expected in such an event, but with a low flux that may be ~~di�fficult~~ to detect.		emission. A GRB is expected in such an event, but with a low flux that may be difficult to detect.


	== Observational Constraints ==		== Observational Constraints ==
	A core-collapse supernova is expected to be coincident with the FRB.		A core-collapse supernova is expected to be coincident with the FRB.

Emma Platts at 12:17, 26 September 2018

2018-09-26T12:17:12Z

← Older revision		Revision as of 08:17, 26 September 2018
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	\|Progenitor = NS-SN Interaction		\|Progenitor = NS-SN Interaction
	\|Type = Single		\|Type = Single
	\|EnergyMechanism = Mag. ~~reconnect.~~		\|EnergyMechanism = Mag. reconnection
	\|EmissionMechanism = --		\|EmissionMechanism = --
	\|LFRadioCounterpart = Yes		\|LFRadioCounterpart = Yes

Shriharsh at 02:21, 26 September 2018

2018-09-26T02:21:59Z

← Older revision		Revision as of 22:21, 25 September 2018
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	== Model Description ==		== Model Description ==
	A supernova ~~explosion~~ in a ~~neutron star~~ binary ~~can lead to~~ the shock ~~wave interacting with~~ the ~~companion neutron star's~~ magnetosphere, ~~leading~~ to ~~a FRB~~.
			This theory posits that an FRB could be formed when a supernova shock interacts
			with the magnetosphere of a NS in a binary system. When the shock encounters the NS
			magnetosphere, it sweeps out a magnetospheric tail, which triggers reconnection and hence
			emission. A GRB is expected in such an event, but with a low flux that may be di�fficult to detect.


	== Observational Constraints ==		== Observational Constraints ==
	A core-collapse supernova is expected to be coincident with the FRB.		A core-collapse supernova is expected to be coincident with the FRB.

Shriharsh: Created page with " {{FRBTableTemplate |Category = Shock Inte..."

2018-09-26T01:15:06Z

Created page with "   {{FRBTableTemplate |Category = Shock Inte..."

New page

{{FRBTableTemplate
|Category = Shock Interaction
|Progenitor = NS-SN Interaction
|Type = Single
|EnergyMechanism = Mag. reconnect.
|EmissionMechanism = --
|LFRadioCounterpart = Yes
|HFRadioCounterpart = --
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = Supernova
|XrayCounterpart = --
|GammarayCounterpart = --
|GWCounterpart = --
|NeutrinoCounterpart = --
|References = http://adsabs.harvard.edu/abs/2009AstL...35..241E
|Comments =
}}

== Model Description ==
A supernova explosion in a neutron star binary can lead to the shock wave interacting with the companion neutron star's magnetosphere, leading to a FRB.

== Observational Constraints ==
A core-collapse supernova is expected to be coincident with the FRB.