NS-SN Interaction: Difference between revisions

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|OIRCounterpart        = Supernova
|OIRCounterpart        = Supernova
|XrayCounterpart        = --
|XrayCounterpart        = --
|GammarayCounterpart    = --
|GammarayCounterpart    = possible GRB (low flux)
|GWCounterpart          = --
|GWCounterpart          = --
|NeutrinoCounterpart    = --
|NeutrinoCounterpart    = --
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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.

Latest revision as of 08:40, 10 October 2018





Summary Table
Category Progenitor Type Energy Mechanism Emission Mechanism Counterparts References Brief Comments
LF Radio HF Radio Microwave Terahertz Optical/IR X-rays Gamma-rays Gravitational Waves Neutrinos
Shock Interaction NS-SN Interaction Single Mag. reconnection -- Yes -- -- -- Supernova -- possible GRB (low flux) -- -- http://adsabs.harvard.edu/abs/2009AstL...35..241E

Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)


Model Description

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.

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.