KNBH-BH (Inspiral): Difference between revisions
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|EmissionMechanism = Curv. | |EmissionMechanism = Curv. | ||
|LFRadioCounterpart = Yes | |LFRadioCounterpart = Yes | ||
|HFRadioCounterpart = | |HFRadioCounterpart = Afterglow | ||
|MicrowaveCounterpart = -- | |MicrowaveCounterpart = -- | ||
|THzCounterpart = -- | |THzCounterpart = -- | ||
|OIRCounterpart = -- | |OIRCounterpart = -- | ||
|XrayCounterpart = | |XrayCounterpart = Yes | ||
|GammarayCounterpart = sGRB <br/> if jet aligned | |GammarayCounterpart = sGRB <br/> if jet aligned | ||
|GWCounterpart = Yes | |GWCounterpart = Yes | ||
|NeutrinoCounterpart = -- | |NeutrinoCounterpart = -- | ||
|References = | |References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1602.04542 | ||
|Comments = Unlikely to account for full FRB population. | |Comments = Unlikely to account for full FRB population. | ||
}} | }} | ||
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== Model Description == | == Model Description == | ||
A binary BH system in which at least one of the spinning BHs carries a charge would induce a global magnetic dipole normal to the orbital plane. During inspiral, as the orbital separation decreases, the magnetic flux of the system changes rapidly, which leads to particle bunching and the emission of coherent curvature radiation | A binary BH system in which at least one of the spinning BHs carries a charge would induce a global magnetic dipole normal to the orbital plane. During inspiral, as the orbital separation decreases, the magnetic flux of the system changes rapidly, which leads to particle bunching and the emission of coherent curvature radiation. | ||
== Observational Constraints == | == Observational Constraints == | ||
For some minimal values of the charge of the BH, this scenario could produce an FRB and a sGRB. The detection of both signals could provide a lower limit on the charge, and the non-detection of a sGRB could provide an upper limit. | |||
Latest revision as of 04:37, 11 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 | KNBH-BH | Single | Mag. flux change | Curv. | Yes | Afterglow | -- | -- | -- | Yes | sGRB if jet aligned |
Yes | -- | http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1602.04542 | Unlikely to account for full FRB population. |
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
Model Description
A binary BH system in which at least one of the spinning BHs carries a charge would induce a global magnetic dipole normal to the orbital plane. During inspiral, as the orbital separation decreases, the magnetic flux of the system changes rapidly, which leads to particle bunching and the emission of coherent curvature radiation.
Observational Constraints
For some minimal values of the charge of the BH, this scenario could produce an FRB and a sGRB. The detection of both signals could provide a lower limit on the charge, and the non-detection of a sGRB could provide an upper limit.