NS to KNBH: Difference between revisions
Jump to navigation
Jump to search
Emma Platts (talk | contribs) No edit summary |
Emma Platts (talk | contribs) No edit summary |
||
| (2 intermediate revisions by the same user not shown) | |||
| Line 14: | Line 14: | ||
|THzCounterpart = -- | |THzCounterpart = -- | ||
|OIRCounterpart = -- | |OIRCounterpart = -- | ||
|XrayCounterpart = | |XrayCounterpart = Possible afterglow | ||
|GammarayCounterpart = | |GammarayCounterpart = Possible GRB | ||
|GWCounterpart = Yes | |GWCounterpart = Yes | ||
|NeutrinoCounterpart = -- | |NeutrinoCounterpart = -- | ||
|References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1307.1409, http://adsabs.harvard.edu/ | |References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1307.1409, http://adsabs.harvard.edu/abs/2014ApJ...780L..21Z, http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1603.05509 | ||
|Comments = Possible X-ray afterglow and a short/long GRB created in NS birth prior to the FRB. | |Comments = Possible X-ray afterglow and a short/long GRB created in NS birth prior to the FRB. | ||
}} | }} | ||
Latest revision as of 04:54, 17 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 | |||||||
| Collapse | NS to KNBH | Single | Mag. reconnection | Curv. | Yes | -- | -- | -- | -- | Possible afterglow | Possible GRB | Yes | -- | http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1307.1409, http://adsabs.harvard.edu/abs/2014ApJ...780L..21Z, http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1603.05509 | Possible X-ray afterglow and a short/long GRB created in NS birth prior to the FRB. |
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
Model Description
Upon the collapse of a supramassive NS into a NKBH, an event horizon will likely form before most of the mass and radiation can escape. By the no-hair theorem, magnetic fields are forbidden from piercing the event horizon, and so the magnetosphere will be left behind. Alternatively, if a NS collapses into a metastable KNBH, its electric discharge can cause the magnetosphere to be shed. Violent magnetic reconnection outside the horizon would then induce a strong magnetic shock wave that moves through the remaining plasma at the speed of light, resulting in a single FRB.
Observational Constraints
--