NS-SN Interaction: Difference between revisions
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|Progenitor = NS-SN Interaction | |Progenitor = NS-SN Interaction | ||
|Type = Single | |Type = Single | ||
|EnergyMechanism = Mag. | |EnergyMechanism = Mag. reconnection | ||
|EmissionMechanism = -- | |EmissionMechanism = -- | ||
|LFRadioCounterpart = Yes | |LFRadioCounterpart = Yes | ||
| Line 15: | Line 15: | ||
|OIRCounterpart = Supernova | |OIRCounterpart = Supernova | ||
|XrayCounterpart = -- | |XrayCounterpart = -- | ||
|GammarayCounterpart = | |GammarayCounterpart = possible GRB (low flux) | ||
|GWCounterpart = -- | |GWCounterpart = -- | ||
|NeutrinoCounterpart = -- | |NeutrinoCounterpart = -- | ||
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== Model Description == | == 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 == | == Observational Constraints == | ||
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 07:40, 10 October 2018
| 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.