NS-NS Merger (Mag. Reconnection): Difference between revisions
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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 | ||
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== 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. 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. | ||
Latest revision as of 05:36, 9 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 | |||||||
| Merger | NS-NS | Both | Mag. reconnection | Curv. | Yes (excl. self absorption) | Yes | ? | ? | Kilonova | Afterglow | sGRB if jet aligned |
Yes | -- | http://adsabs.harvard.edu/abs/2016ApJ...822L...7W | None |
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
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. In this theory, the merger product is presumed to be a rapidly spinning BH.
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.