https://frbtheorycat.org/api.php?action=feedcontributions&user=Apw&feedformat=atomFRB Theory Wiki - User contributions [en]2024-03-29T11:40:56ZUser contributionsMediaWiki 1.39.6https://frbtheorycat.org/index.php?title=Starquakes&diff=234Starquakes2018-10-10T13:13:19Z<p>Apw: </p>
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{{FRBTableTemplate<br />
|Category = Other<br />
|Progenitor = Starquakes<br />
|Type = Repeat<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = Yes<br />
|GammarayCounterpart = Yes <br/> if jet aligned<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2018ApJ...852..140W<br />
|Comments = None<br />
}}<br />
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== Model Description ==<br />
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The starquakes of a pulsar have been considered as a source of repeating FRBs. The bursts of FRB 121102 are consistent with the aftershock sequence of an earthquake, where the burst’s time-decaying rate of seismicity falls within the typical values of earthquakes. They also show that the burst energy distribution of FRB 121102 has a power law form, much like that of the Gutenberg-Richter law of earthquakes. Further, the waiting time of bursts has a Gaussian distribution; another characteristic feature of earthquakes. <br />
<br />
== Observational Constraints ==<br />
<br />
Starquakes are poorly understood, limiting the testability of this theory. They may be associated with SGRs, which offers counterparts for which to search.</div>Apwhttps://frbtheorycat.org/index.php?title=Small_Body_and_Pulsar&diff=233Small Body and Pulsar2018-10-10T12:57:42Z<p>Apw: </p>
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{{FRBTableTemplate<br />
|Category = Collision / Interaction<br />
|Progenitor = Small Body and Pulsar<br />
|Type = Single<br />
|EnergyMechanism = Maser<br />
|EmissionMechanism = Synch.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2014A%26A...569A..86M<br />
|Comments = None<br />
}}<br />
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== Model Description ==<br />
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<br />
If an orbiting body is massive enough to survive a close encounter without evaporation or breaking up (such as a planet or white dwarf), the highly magnetized pulsar wind will induce an electromagnetic field around the body. In this situation, Alfven wings are created as the pulsar wind combs the field lines from the nearest pole of the orbiting body and into space. The Alfven wings destabilize the plasma near the body’s surface to excite coherent emission. Far from the pulsar companion, the emission is convected with the wind traveling relativistically along the Alfven wings to form a synchrotron maser, whose emission is consistent with FRBs. <br />
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== Observational Constraints ==<br />
<br />
The emission is only observable when the companion is aligned between the pulsar and Earth, and thus should repeat periodically. The signal would be composed of one to four peaks, a few milliseconds each, with an event duration less than a few seconds. No emission counterparts are expected, as synchrotron emission from a hot plasma component would be incoherent and thus too weak.</div>Apwhttps://frbtheorycat.org/index.php?title=NS-WD_Merger&diff=232NS-WD Merger2018-10-10T12:47:28Z<p>Apw: </p>
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{{FRBTableTemplate<br />
|Category = Merger<br />
|Progenitor = NS-WD<br />
|Type = Single<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes <br />
|HFRadioCounterpart = Yes <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/abs/1712.03509<br />
|Comments = <br />
}}<br />
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== Model Description ==<br />
Upon NS-WD coalescence, magnetic reconnection injects relativistic electrons from the surface of the WD into the magnetosphere of the NS to create an FRB. The timescale of the burst is assumed to be from the time of electron injection to the formation of the final merged object. It is predicted that the shorter the intrinsic width of the FRB, the higher the flux density.<br />
<br />
== Observational Constraints ==<br />
<br />
Of the 28 FRBs analysed (those available at the time), the pulse widths were broader than expected in the NS-WD scenario, but perhaps pulse widths vary more widely between FRBs due to multipath scattering through the IGM.</div>Apwhttps://frbtheorycat.org/index.php?title=NS-WD_Merger&diff=231NS-WD Merger2018-10-10T12:46:46Z<p>Apw: </p>
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<!-- Brings in the summary table --><br />
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{{FRBTableTemplate<br />
|Category = Merger<br />
|Progenitor = NS-WD<br />
|Type = Single<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes <br />
|HFRadioCounterpart = Yes <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/abs/1712.03509<br />
|Comments = <br />
}}<br />
<br />
== Model Description ==<br />
Upon NS-WD coalescence, magnetic reconnection injects relativistic electrons from the surface of the WD into the magnetosphere of the NS to create an FRB.<br />
<br />
== Observational Constraints ==<br />
<br />
The timescale of the burst is assumed to be from the time of electron injection to the formation of the final merged object. It is predicted that the shorter the intrinsic width of the FRB, the higher the flux density. Of the 28 FRBs analysed (those available at the time), the pulse widths were broader than expected in the NS-WD scenario, but perhaps pulse widths vary more widely between FRBs due to multipath scattering through the IGM.</div>Apwhttps://frbtheorycat.org/index.php?title=NS-WD_Accretion&diff=230NS-WD Accretion2018-10-10T12:45:00Z<p>Apw: </p>
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{{FRBTableTemplate<br />
|Category = Accretion<br />
|Progenitor = NS-WD<br />
|Type = Repeating<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes <br />
|HFRadioCounterpart = Yes <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = Yes, but unlikely detectable<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2016ApJ...823L..28G<br />
|Comments = <br />
}}<br />
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== Model Description ==<br />
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This model considers the interaction between the bipolar magnetic fields of a NS and a magnetic white dwarf (WD) as a possible origin of<br />
repeating FRBs. As the WD exceeds its Roche lobe, the NS accretes the infalling matter. Upon their approach, the magnetized materials may trigger magnetic reconnection<br />
and emit curvature radiation. In a rapidly rotating neutron star, the angular momentum added by accretion is lost to gravitational radiation, but the mass transfer may be violent<br />
enough for the angular momentum of the WD to dominate over the gravitational radiation. In this case, the WD is kicked away from the NS, and the process of accretion, and thus<br />
magnetic reconnection, may repeat. The timescale of emission is assumed to be the same as that of magnetic reconnection, and the time interval between adjacent bursts is derived<br />
from its relationship to the mass transferred by the burst.<br />
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== Observational Constraints ==<br />
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Counterparts to this model are not specified, other than to say that possible gamma-ray emission from synchrotron radiation is unlikely detectable.</div>Apwhttps://frbtheorycat.org/index.php?title=NS-SN_Interaction&diff=229NS-SN Interaction2018-10-10T12:40:13Z<p>Apw: </p>
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{{FRBTableTemplate<br />
|Category = Shock Interaction<br />
|Progenitor = NS-SN Interaction <br />
|Type = Single<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = --<br />
|LFRadioCounterpart = Yes <br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = Supernova<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = possible GRB (low flux)<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2009AstL...35..241E<br />
|Comments = <br />
}}<br />
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== Model Description ==<br />
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This theory posits that an FRB could be formed when a supernova shock interacts<br />
with the magnetosphere of a NS in a binary system. When the shock encounters the NS<br />
magnetosphere, it sweeps out a magnetospheric tail, which triggers reconnection and hence<br />
emission.<br />
<br />
== Observational Constraints ==<br />
<br />
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.</div>Apwhttps://frbtheorycat.org/index.php?title=NS_and_Primordial_BH&diff=228NS and Primordial BH2018-10-10T12:35:34Z<p>Apw: /* Model Description */</p>
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{{FRBTableTemplate<br />
|Category = Collision / Interaction<br />
|Progenitor = NS and Primordial BH<br />
|Type = Both<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = --<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = Yes<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/pdf/1704.05931.pdf<br />
|Comments = None<br />
}}<br />
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== Model Description ==<br />
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As a PBH passes through a NS, the gravitational drag from the dense NS matter causes the PBH to slow down. The PBH will pass through the middle of the NS and, after losing sufficient kinetic energy, will be pulled back. The PBH will oscillate a few times before settling at the center of the NS. Here, the PBH will begin to accrete the NS until it is swallowed, causing the NS magnetosphere to be shed. The resulting magnetic reconnection releases an FRB. A repeating FRB may also be accounted for in this scenario: a small PBH will take longer to accrete the NS; as the NS is gradually consumed, multiple bundles of magnetic field lines within the NS may be reconfigured, causing multiple bursts.<br />
<br />
== Observational Constraints ==<br />
<br />
Gravitational waves are expected counterparts, but may not be detectable at cosmological distances. The model can account multiple peaks, polarized emission and Faraday rotation.</div>Apwhttps://frbtheorycat.org/index.php?title=NS_and_Primordial_BH&diff=227NS and Primordial BH2018-10-10T12:32:55Z<p>Apw: </p>
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{{FRBTableTemplate<br />
|Category = Collision / Interaction<br />
|Progenitor = NS and Primordial BH<br />
|Type = Both<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = --<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = Yes<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/pdf/1704.05931.pdf<br />
|Comments = None<br />
}}<br />
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== Model Description ==<br />
<br />
FRBs may result from interactions between NSs and primordial black holes (PBHs). As a PBH passes through a NS, the gravitational drag from the dense NS matter causes the PBH to slow down. The PBH will pass through the middle of the NS and, after losing sufficient kinetic energy, will be pulled back. The PBH will oscillate a few times before settling at the center of the NS. Here, the PBH will begin to accrete the NS until it is swallowed, causing the NS magnetosphere to be shed. The resulting magnetic reconnection releases an FRB. A repeating FRB may also be accounted for in this scenario: a small PBH will take longer to accrete the NS; as the NS is gradually consumed, multiple bundles of magnetic field lines within the NS may be reconfigured, causing multiple bursts.<br />
<br />
== Observational Constraints ==<br />
<br />
Gravitational waves are expected counterparts, but may not be detectable at cosmological distances. The model can account multiple peaks, polarized emission and Faraday rotation.</div>Apwhttps://frbtheorycat.org/index.php?title=NS_and_Primordial_BH&diff=226NS and Primordial BH2018-10-10T12:28:27Z<p>Apw: </p>
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<!-- Brings in the summary table --><br />
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{{FRBTableTemplate<br />
|Category = Collision / Interaction<br />
|Progenitor = NS and Primordial BH<br />
|Type = Both<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = --<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = Yes<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/pdf/1704.05931.pdf<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
FRBs may result from interactions between NSs and primordial black holes (PBHs). As a primordial black hole (PBH) passes through a NS, the gravitational drag from the dense NS matter causes the PBH to slow down. The PBH will pass through the middle of the NS and, after losing sufficient kinetic energy, will be pulled back. The PBH will oscillate a few times before settling at the center of the NS. Here, the PBH will begin to accrete the NS until it is swallowed, causing the NS magnetosphere to be shed. The resulting magnetic reconnection releases an FRB. A repeating FRB may also be accounted for in this scenario: a small PBH will take longer to accrete the NS; as the NS is gradually consumed, multiple bundles of magnetic field lines within the NS may be reconfigured, causing multiple bursts.<br />
<br />
== Observational Constraints ==<br />
<br />
Gravitational waves are expected counterparts, but may not be detectable at cosmological distances. The model can account multiple peaks, polarized emission and Faraday rotation.</div>Apwhttps://frbtheorycat.org/index.php?title=NS_and_Asteroids/Comets&diff=223NS and Asteroids/Comets2018-10-10T11:31:02Z<p>Apw: </p>
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{{FRBTableTemplate<br />
|Category = Collision/ Interaction<br />
|Progenitor = NS and Asteroids/ Comets<br />
|Type = Single<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = Yes (probably too faint to detect)<br />
|GammarayCounterpart = Yes (probably too faint to detect)<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2015ApJ...809...24G<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
A small body, such as a comet or asteroid, captured by the gravitational potential of a NS will free-fall toward it, becoming radially elongated until it exceeds its Roche limit and breaks apart. The fragments are compressed by the gravitational acceleration and the magnetic field of the NS, resulting in leading and lagging portions with the same velocity. In order to nullify the effects evaporation and ionisation may have, the body must have a sufficiently large mass and shear, and is thus predicted to be of Fe-Ni composition. Infalling matter would be confined to the poles of the NS by strong magnetic stresses, creating an accretion column. If the accretion column travels through a region where electrostatic equilibrium has been disturbed, particles are accelerated to yield γ-ray emission. When the matter impacts the NS, an expanding plasmoid fireball will be launched along the magnetic field lines. Magnetic reconnection at the collision site accelerates e+/e− pairs within the plasma-fan to ultra-relativistic speeds, resulting in coherent curvature emission.<br />
<br />
== Observational Constraints ==<br />
<br />
The event rate associated with such a theory has been shown to be consistent with the other predictions and, notably, the impact timescale between the leading and tailing fragments is roughly consistent with the brevity of FRB signals. The model predicts X-ray emission and γ-ray emission from inverse Compton scattering, however these are probably too faint to be observed.</div>Apwhttps://frbtheorycat.org/index.php?title=NS_and_Asteroids/Comets&diff=222NS and Asteroids/Comets2018-10-10T11:28:48Z<p>Apw: </p>
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<!-- Brings in the summary table --><br />
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{{FRBTableTemplate<br />
|Category = Collision/ Interaction<br />
|Progenitor = NS and Asteroids/ Comets<br />
|Type = Single<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2015ApJ...809...24G<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
A small body, such as a comet or asteroid, captured by the gravitational potential of a NS will free-fall toward it, becoming radially elongated until it exceeds its Roche limit and breaks apart. The fragments are compressed by the gravitational acceleration and the magnetic field of the NS, resulting in leading and lagging portions with the same velocity. In order to nullify the effects evaporation and ionisation may have, the body must have a sufficiently large mass and shear, and is thus predicted to be of Fe-Ni composition. Infalling matter would be confined to the poles of the NS by strong magnetic stresses, creating an accretion column. If the accretion column travels through a region where electrostatic equilibrium has been disturbed, particles are accelerated to yield γ-ray emission. When the matter impacts the NS, an expanding plasmoid fireball will be launched along the magnetic field lines. Magnetic reconnection at the collision site accelerates e+/e− pairs within the plasma-fan to ultra-relativistic speeds, resulting in coherent curvature emission.<br />
<br />
== Observational Constraints ==<br />
<br />
The event rate associated with such a theory has been shown to be consistent with the other predictions and, notably, the impact timescale between the leading and tailing fragments is roughly consistent with the brevity of FRB signals. The model predicts X-ray emission and γ-ray emission from inverse Compton scattering, however these are probably too faint to be observed.</div>Apwhttps://frbtheorycat.org/index.php?title=NS_and_Asteroid_Belt&diff=221NS and Asteroid Belt2018-10-10T11:22:07Z<p>Apw: </p>
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<!-- Brings in the summary table --><br />
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{{FRBTableTemplate<br />
|Category = Collision/ Interaction<br />
|Progenitor = NS and Asteroid Belt<br />
|Type = Repeat<br />
|EnergyMechanism = Electron stripping<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = --<br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = Yes<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2016ApJ...829...27D<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
Consider an asteroid belt surrounding a star. If a pulsar passes through this system, it is likely to encounter multiple asteroids. When this happens, charged particles may be stripped from the asteroidal surface into the NS magnetosphere, where they are accelerated to ultra-relativistic speeds, resulting in coherent curvature radiation. <br />
<br />
== Observational Constraints ==<br />
<br />
The time between edge on collisions within the asteroid belt is consistent with the time between the signals of FRB 121102.</div>Apwhttps://frbtheorycat.org/index.php?title=Neutral_Cosmic_Strings&diff=220Neutral Cosmic Strings2018-10-10T11:10:46Z<p>Apw: </p>
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<!-- Brings in the summary table --><br />
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{{FRBTableTemplate<br />
|Category = Other<br />
|Progenitor = Neutral Cosmic Strings<br />
|Type = Single<br />
|EnergyMechanism = Cusp decay<br />
|EmissionMechanism = --<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = GRB <br/> if jet aligned<br />
|GWCounterpart = Yes<br />
|NeutrinoCounterpart = Yes<br />
|References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1707.02397<br />
|Comments = High energy cosmic rays are also expected.<br />
}}<br />
<br />
== Model Description ==<br />
<br />
Nambu-Goto (infinitely thin, idealised) cosmic strings generically form cusps, portions of the string which fold back onto themselves and move at the speed of light. The cusps decay, emitting a beam of coherent radiation. The decay particle can ostensibly be of any energy and frequency range, and so should extend down into radio bursts. <br />
<br />
== Observational Constraints ==<br />
<br />
The event rate, timescale, and flux emitted are shown to be consistent with FRB data, however the relativistic effects on the cusp shape was not factored in. By taking this into account, cusp decay is in fact incompatible with current FRB data. Cosmic strings are not ruled out by observations, and would necessarily include counterparts of other electromagnetic frequencies, specifically, GRBs, cosmic rays and neutrinos, and GWs.</div>Apwhttps://frbtheorycat.org/index.php?title=Neutral_Cosmic_Strings&diff=219Neutral Cosmic Strings2018-10-10T11:09:47Z<p>Apw: </p>
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<div><br />
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<!-- Brings in the summary table --><br />
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{{FRBTableTemplate<br />
|Category = Other<br />
|Progenitor = Neutral Cosmic Strings<br />
|Type = Single<br />
|EnergyMechanism = Cusp decay<br />
|EmissionMechanism = --<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = GRB <br/> if jet aligned<br />
|GWCounterpart = Yes<br />
|NeutrinoCounterpart = Yes<br />
|References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1707.02397<br />
|Comments = High energy cosmic rays are also expected.<br />
}}<br />
<br />
== Model Description ==<br />
<br />
Nambu-Goto (infinitely thin, idealised) cosmic strings generically form cusps, portions of the string which fold back onto themselves and move at the speed of light. The cusps decay, emitting a beam of coherent radiation. The decay particle can ostensibly be of any energy and frequency range, and so should extend down into radio bursts. Cusp decay from cosmic strings has been put forward to explain FRBs [285]. <br />
<br />
== Observational Constraints ==<br />
<br />
The event rate, timescale, and flux emitted are shown to be consistent with FRB data, however the relativistic effects on the cusp shape was not factored in. By taking this into account, cusp decay is in fact incompatible with current FRB data. Cosmic strings are not ruled out by observations, and would necessarily include counterparts of other electromagnetic frequencies, specifically, GRBs, cosmic rays and neutrinos, and GWs.</div>Apwhttps://frbtheorycat.org/index.php?title=Neutral_Cosmic_Strings&diff=218Neutral Cosmic Strings2018-10-10T11:05:23Z<p>Apw: </p>
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<div><br />
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<!-- Brings in the summary table --><br />
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{{FRBTableTemplate<br />
|Category = Other<br />
|Progenitor = Neutral Cosmic Strings<br />
|Type = Single<br />
|EnergyMechanism = Cusp decay<br />
|EmissionMechanism = --<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = GRB <br/> if jet aligned<br />
|GWCounterpart = Yes<br />
|NeutrinoCounterpart = Yes<br />
|References = https://arxiv.org/pdf/1701.01109.pdf<br />
|Comments = High energy cosmic rays are also expected.<br />
}}<br />
<br />
== Model Description ==<br />
<br />
Nambu-Goto (infinitely thin, idealised) cosmic strings generically form cusps, portions of the string which fold back onto themselves and move at the speed of light. The cusps decay, emitting a beam of coherent radiation. The decay particle can ostensibly be of any energy and frequency range, and so should extend down into radio bursts. Cusp decay from cosmic strings has been put forward to explain FRBs [285]. The event rate, timescale, and flux emitted are shown to be consistent with FRB data, however the relativistic effects on the cusp shape was not factored in. By taking this into account, cusp decay is in fact incompatible with current FRB data [286]. Cosmic strings are not ruled out by observations, and would necessarily include counterparts of other electromagnetic frequencies—specifically, GRBs [287], cosmic rays [288] and neutrinos [289]—and GWs.<br />
<br />
== Observational Constraints ==<br />
<br />
To be filled in with updated draft</div>Apwhttps://frbtheorycat.org/index.php?title=KNBH-BH_(Inspiral)&diff=217KNBH-BH (Inspiral)2018-10-10T10:56:52Z<p>Apw: /* Observational Constraints */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Merger<br />
|Progenitor = KNBH-BH<br />
|Type = Single<br />
|EnergyMechanism = Mag. flux change<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = Afterglow <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = Yes<br />
|GammarayCounterpart = sGRB <br/> if jet aligned<br />
|GWCounterpart = Yes<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/pdf/1602.04542.pdf<br />
|Comments = Unlikely to account for full FRB population.<br />
}}<br />
<br />
== Model Description ==<br />
<br />
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.<br />
<br />
== Observational Constraints ==<br />
<br />
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.</div>Apwhttps://frbtheorycat.org/index.php?title=KNBH-BH_(Inspiral)&diff=216KNBH-BH (Inspiral)2018-10-10T10:56:27Z<p>Apw: /* Model Description */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Merger<br />
|Progenitor = KNBH-BH<br />
|Type = Single<br />
|EnergyMechanism = Mag. flux change<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = Afterglow <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = Yes<br />
|GammarayCounterpart = sGRB <br/> if jet aligned<br />
|GWCounterpart = Yes<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/pdf/1602.04542.pdf<br />
|Comments = Unlikely to account for full FRB population.<br />
}}<br />
<br />
== Model Description ==<br />
<br />
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.<br />
<br />
== Observational Constraints ==</div>Apwhttps://frbtheorycat.org/index.php?title=Jet-Caviton&diff=215Jet-Caviton2018-10-10T10:50:47Z<p>Apw: </p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = AGN<br />
|Progenitor = Jet-Caviton Interaction<br />
|Type = Both<br />
|EnergyMechanism = Electron scattering<br />
|EmissionMechanism = Bremsst.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = Yes <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = Possible GRB<br />
|GWCounterpart = Yes<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2016PhRvD..93b3001R, https://arxiv.org/pdf/1704.08097.pdf<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
Let us first discuss the formation of AGN jets. Consider a hot accretion disk formed as matter is captured and spirals into a moderately sized BH. Some of the in-falling gas and dust is confined to the poles and ejected in two relativistic jets [229]. Hot gas clouds of varying densities surround the BH, forming a toroid that extends a few parsecs from the BH. As the AGN jet interacts with the clouds, it becomes narrowly collimated. The relativistic e+/e− beam encounters material at the center of the host galaxy, and strong turbulence is produced by plasma instabilities. The total pressure and the ponderomotive force (experienced by a charged particle in an oscillating electric field) cause electrons and ions to separate. These regions, called cavitons, are filled by a strong electrostatic field. Electrons from the beam that pass through the caviton are coherently scattered and emit strongly beamed Bremsstrahlung radiation in pulses. FRBs may be single or repeating. <br />
<br />
<br />
== Observational Constraints ==<br />
<br />
Radiation might be linearly polarized if there is a local magnetic field, however the 100% polarization degree of FRB 121102 would be difficult to account for in this scenario. The persistent scintillating radio emission from the AGN is an expected counterpart, which agrees with observations of FRB 121102.</div>Apwhttps://frbtheorycat.org/index.php?title=DSR_in_Galaxies&diff=214DSR in Galaxies2018-10-10T10:41:28Z<p>Apw: /* Model Description */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Other<br />
|Progenitor = Dicke's Superradiance in Galaxies<br />
|Type = Both<br />
|EnergyMechanism = Dicke's Superradiance<br />
|EmissionMechanism = Synch.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2018MNRAS.475..514H<br />
|Comments = --<br />
}}<br />
<br />
== Model Description ==<br />
<br />
Postulated in 1953 and first detected in 1973, Dicke's Superradiance (DSR) has been invoked as one of the few “microphysical” FRB models. The aim is to explain FRBs using the atomic interactions in galaxies. DSR can occur in astrophysical settings, provided: the collection of atoms is inverted; the velocity coherence is high; and the non-coherent relaxation mechanisms occur on a timescale larger than the delay time. If one models the ISM as a cylinder of atoms, the predicted DSR emission power and timescale can fit FRB data. This model is additionally appealing since the DSR mechanism can adapt to a wide variety of FRB behaviour, and proposes no new entities/physics. Indeed, the DMs associated with FRBs fits well with the ISM required for DSR to occur. DSR also presents a mechanism through which a repeater can be explained. If a collection of molecules has DSR triggered at the same time, the intrinsic variation in the DSR timescale and time delay would give the observation of bursts at different times. The variation is because the time delay is an expectation value, and the collection of molecules being ionised at the same time is due to the entanglement, which also causes a differential in emission time. This process can happen repeatedly as population inversion will be non-inverted but swiftly restored via the ISM, which will drive more FRB pulses, and so on. The flux distribution of such a setup can be matched to FRB 121102.<br />
<br />
== Observational Constraints ==</div>Apwhttps://frbtheorycat.org/index.php?title=DSR_in_Galaxies&diff=213DSR in Galaxies2018-10-10T10:39:05Z<p>Apw: </p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Other<br />
|Progenitor = Dicke's Superradiance in Galaxies<br />
|Type = Both<br />
|EnergyMechanism = Dicke's Superradiance<br />
|EmissionMechanism = Synch.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2018MNRAS.475..514H<br />
|Comments = --<br />
}}<br />
<br />
== Model Description ==<br />
<br />
Postulated in 1953 and first detected in 1973, Dicke's Superradiance (DSR) has been invoked as one of the few “microphysical” FRB models. The aim is to explain FRBs using the atomic interactions in galaxies. DSR can occur in astrophysical settings, provided: the collection of atoms is inverted (to wit, a majority of atoms exist in higher excited states than the minority); the velocity coherence is high; and the non-coherent relaxation mechanisms occur on a timescale larger than the delay time. If one models the ISM as a cylinder of atoms, the predicted DSR emission power and timescale can fit FRB data. This is because the coherent behaviour of the DSR atoms has a timescale which scales as τ ∝ N−1 and an intensity which scales as I ∝ N2, where N is the number of entangled molecules. This model is additionally appealing since the DSR mechanism can adapt to a wide variety of FRB behaviour, and proposes no new entities/physics. Indeed, the DMs associated with FRBs fits well with the ISM required for DSR to occur. DSR also presents a mechanism through which a repeater can be explained. If a collection of molecules has DSR triggered at the same time, the intrinsic variation in the DSR timescale and time delay would give the observation of bursts at different times. The variation is because the time delay is an expectation value, and the collection of molecules being ionised at the same time is due to the entanglement, which also causes a differential in emission time. This process can happen repeatedly as population inversion will be non-inverted but swiftly restored via the ISM, which will drive more FRB pulses, and so on. The flux distribution of such a setup can be matched to FRB 121102.<br />
<br />
== Observational Constraints ==</div>Apwhttps://frbtheorycat.org/index.php?title=Axion_Star_and_BH&diff=212Axion Star and BH2018-10-10T10:27:41Z<p>Apw: /* Model Description */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Collision / Interaction<br />
|Progenitor = Axion Star and BH<br />
|Type = Repeat<br />
|EnergyMechanism = Electron oscillation<br />
|EmissionMechanism = --<br />
|LFRadioCounterpart = Yes (Circular Polarization)<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/pdf/1707.04827.pdf<br />
|Comments = <br />
}}<br />
<br />
== Model Description ==<br />
<br />
If an axion star were captured by a BH with a strongly magnetized accretion disk, the axion star’s orbit will lead it to approach and impact the accretion disk several times at different locations. The electric field induced by the axion star passing through a strong magnetic field will result in the coherent oscillation of surrounding electrons. The axion star will likely make several impacts before evaporating or eventually being absorbed by the BH.<br />
<br />
== Observational Constraints ==<br />
<br />
The frequency of the radiation will depend on the velocity of the accretion disk at the point of impact. In this way, the variation in central burst frequencies of FRB 121102 can be explained. The intrinsic emission frequency is finite, FRBs would be circularly polarized, and no counterparts are expected.</div>Apwhttps://frbtheorycat.org/index.php?title=Axion_Star_and_BH&diff=211Axion Star and BH2018-10-10T10:27:22Z<p>Apw: /* Observational Constraints */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Collision / Interaction<br />
|Progenitor = Axion Star and BH<br />
|Type = Repeat<br />
|EnergyMechanism = Electron oscillation<br />
|EmissionMechanism = --<br />
|LFRadioCounterpart = Yes (Circular Polarization)<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/pdf/1707.04827.pdf<br />
|Comments = <br />
}}<br />
<br />
== Model Description ==<br />
<br />
If an axion star were captured by a BH with a strongly magnetized accretion disk, the axion star’s orbit will lead it to approach and impact the accretion disk several times at different locations. The electric field induced by the axion star passing through a strong magnetic field will result in the coherent oscillation of surrounding electrons.<br />
<br />
== Observational Constraints ==<br />
<br />
The frequency of the radiation will depend on the velocity of the accretion disk at the point of impact. In this way, the variation in central burst frequencies of FRB 121102 can be explained. The intrinsic emission frequency is finite, FRBs would be circularly polarized, and no counterparts are expected.</div>Apwhttps://frbtheorycat.org/index.php?title=Axion_Star_and_BH&diff=210Axion Star and BH2018-10-10T10:05:30Z<p>Apw: </p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Collision / Interaction<br />
|Progenitor = Axion Star and BH<br />
|Type = Repeat<br />
|EnergyMechanism = Electron oscillation<br />
|EmissionMechanism = --<br />
|LFRadioCounterpart = Yes (Circular Polarization)<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/pdf/1707.04827.pdf<br />
|Comments = <br />
}}<br />
<br />
== Model Description ==<br />
<br />
If an axion star were captured by a BH with a strongly magnetized accretion disk, the axion star’s orbit will lead it to approach and impact the accretion disk several times at different locations. The electric field induced by the axion star passing through a strong magnetic field will result in the coherent oscillation of surrounding electrons.<br />
<br />
== Observational Constraints ==<br />
<br />
The frequency of the radiation will depend on the velocity of the accretion disk at the point of impact. In this way, the variation in central burst frequencies of FRB 121102 can be explained. The axion star will likely make several impacts before evaporating or eventually being absorbed by the BH. The intrinsic emission frequency is finite, FRBs would be circularly polarized, and no counterparts are expected.</div>Apwhttps://frbtheorycat.org/index.php?title=Axion_Star_and_BH&diff=209Axion Star and BH2018-10-10T09:59:18Z<p>Apw: /* Observational Constraints */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Collision / Interaction<br />
|Progenitor = Axion Star and BH<br />
|Type = Repeat<br />
|EnergyMechanism = Electron oscillation<br />
|EmissionMechanism = --<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/pdf/1707.04827.pdf<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
If an axion star were captured by a BH with a strongly magnetized accretion disk, the axion star’s orbit will lead it to approach and impact the accretion disk several times at different locations. The electric field induced by the axion star passing through a strong magnetic field will result in the coherent oscillation of surrounding electrons.<br />
<br />
== Observational Constraints ==<br />
<br />
The frequency of the radiation will depend on the velocity of the accretion disk at the point of impact. In this way, the variation in central burst frequencies of FRB 121102 can be explained. The axion star will likely make several impacts before evaporating or eventually being absorbed by the BH. The intrinsic emission frequency is finite, FRBs would be circularly polarized, and no counterparts are expected.</div>Apwhttps://frbtheorycat.org/index.php?title=Axion_Star_and_BH&diff=208Axion Star and BH2018-10-10T09:59:01Z<p>Apw: /* Model Description */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Collision / Interaction<br />
|Progenitor = Axion Star and BH<br />
|Type = Repeat<br />
|EnergyMechanism = Electron oscillation<br />
|EmissionMechanism = --<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/pdf/1707.04827.pdf<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
If an axion star were captured by a BH with a strongly magnetized accretion disk, the axion star’s orbit will lead it to approach and impact the accretion disk several times at different locations. The electric field induced by the axion star passing through a strong magnetic field will result in the coherent oscillation of surrounding electrons.<br />
<br />
== Observational Constraints ==<br />
<br />
To be filled in with updated draft</div>Apwhttps://frbtheorycat.org/index.php?title=Axion_Quark_Nugget_and_NS&diff=207Axion Quark Nugget and NS2018-10-10T09:47:21Z<p>Apw: /* Observational Constraints */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Collision / Interaction<br />
|Progenitor = Axion Quark Nuggest and NS<br />
|Type = Repeat<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = Possible<br />
|MicrowaveCounterpart = Possible<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/pdf/1806.02352.pdf<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
In close analogy with the axion quark nugget (AQN) mechanism for generating solar nano flares, an AQN falling through an opportunely complicated region in a NS’s magnetosphere may be able to produce sufficient magnetic energy to power FRBs. Shock waves caused by the infalling AQN would trigger magnetic reconnection, and produce a giant flare.<br />
<br />
== Observational Constraints ==<br />
<br />
The predicted event rate is consistent with observations, but the emission timescale (∼ 10 − 100 ms) is larger than what is observed. This discrepancy can be accounted for if the beam moves across the sky, allowing us only a glimpse of the emission. A curvature radiation mechanism is invoked, which predicts a maximum cut-off frequency at infra-red wavelengths; observed counterparts with higher frequencies would invalidate this model. Given the random nature of these events, repeating FRBs would be non-periodic. A correlation between the total energy and duration of the flare is predicted, however because only a fraction of the entire beam would be observed, this relationship would be difficult to verify.</div>Apwhttps://frbtheorycat.org/index.php?title=Axion_Quark_Nugget_and_NS&diff=206Axion Quark Nugget and NS2018-10-10T09:46:51Z<p>Apw: /* Observational Constraints */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Collision / Interaction<br />
|Progenitor = Axion Quark Nuggest and NS<br />
|Type = Repeat<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = Possible<br />
|MicrowaveCounterpart = Possible<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/pdf/1806.02352.pdf<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
In close analogy with the axion quark nugget (AQN) mechanism for generating solar nano flares, an AQN falling through an opportunely complicated region in a NS’s magnetosphere may be able to produce sufficient magnetic energy to power FRBs. Shock waves caused by the infalling AQN would trigger magnetic reconnection, and produce a giant flare.<br />
<br />
== Observational Constraints ==<br />
<br />
The event rate is consistent with observation, but the emission timescale (∼ 10 − 100 ms) is larger than what is observed. This discrepancy can be accounted for if the beam moves across the sky, allowing us only a glimpse of the emission. A curvature radiation mechanism is invoked, which predicts a maximum cut-off frequency at infra-red wavelengths; observed counterparts with higher frequencies would invalidate this model. Given the random nature of these events, repeating FRBs would be non-periodic. A correlation between the total energy and duration of the flare is predicted, however because only a fraction of the entire beam would be observed, this relationship would be difficult to verify.</div>Apwhttps://frbtheorycat.org/index.php?title=Axion_Quark_Nugget_and_NS&diff=205Axion Quark Nugget and NS2018-10-10T09:45:44Z<p>Apw: /* Model Description */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Collision / Interaction<br />
|Progenitor = Axion Quark Nuggest and NS<br />
|Type = Repeat<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = Possible<br />
|MicrowaveCounterpart = Possible<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/pdf/1806.02352.pdf<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
In close analogy with the axion quark nugget (AQN) mechanism for generating solar nano flares, an AQN falling through an opportunely complicated region in a NS’s magnetosphere may be able to produce sufficient magnetic energy to power FRBs. Shock waves caused by the infalling AQN would trigger magnetic reconnection, and produce a giant flare.<br />
<br />
== Observational Constraints ==<br />
<br />
There is a maximum cut-off frequency at infra-red wavelengths, and thus counterparts with higher frequencies would invalidate the model.</div>Apwhttps://frbtheorycat.org/index.php?title=Axion_Minicluster_and_NS&diff=204Axion Minicluster and NS2018-10-10T09:42:23Z<p>Apw: /* Observational Constraints */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Collision / Interaction<br />
|Progenitor = Axion Minicluster and NS<br />
|Type = Single<br />
|EnergyMechanism = Maser<br />
|EmissionMechanism = Synch.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2015JETPL.101....1T<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
Axion clumps with masses below the stellar range, known as Axion Bose Clusters or “miniclusters”, have been considered as FRB progenitors. In the strong magnetic field of a compact object, an instability may arise in a minicluster, causing it to explosively decay into photons via a synchrotron maser mechanism.<br />
<br />
== Observational Constraints ==</div>Apwhttps://frbtheorycat.org/index.php?title=Axion_Minicluster_and_NS&diff=203Axion Minicluster and NS2018-10-10T09:41:46Z<p>Apw: /* Observational Constraints */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Collision / Interaction<br />
|Progenitor = Axion Minicluster and NS<br />
|Type = Single<br />
|EnergyMechanism = Maser<br />
|EmissionMechanism = Synch.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2015JETPL.101....1T<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
Axion clumps with masses below the stellar range, known as Axion Bose Clusters or “miniclusters”, have been considered as FRB progenitors. In the strong magnetic field of a compact object, an instability may arise in a minicluster, causing it to explosively decay into photons via a synchrotron maser mechanism.<br />
<br />
== Observational Constraints ==<br />
<br />
The predicted emission timescale, the energetics, luminosities, and event rate are in-keeping with FRB observations.</div>Apwhttps://frbtheorycat.org/index.php?title=Axion_Minicluster_and_NS&diff=202Axion Minicluster and NS2018-10-10T09:27:40Z<p>Apw: /* Model Description */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Collision / Interaction<br />
|Progenitor = Axion Minicluster and NS<br />
|Type = Single<br />
|EnergyMechanism = Maser<br />
|EmissionMechanism = Synch.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2015JETPL.101....1T<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
Axion clumps with masses below the stellar range, known as Axion Bose Clusters or “miniclusters”, have been considered as FRB progenitors. In the strong magnetic field of a compact object, an instability may arise in a minicluster, causing it to explosively decay into photons via a synchrotron maser mechanism.<br />
<br />
== Observational Constraints ==<br />
<br />
To be filled in with updated draft</div>Apwhttps://frbtheorycat.org/index.php?title=Axion_Minicluster_and_NS&diff=201Axion Minicluster and NS2018-10-10T09:27:11Z<p>Apw: /* Model Description */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Collision / Interaction<br />
|Progenitor = Axion Minicluster and NS<br />
|Type = Single<br />
|EnergyMechanism = Maser<br />
|EmissionMechanism = Synch.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2015JETPL.101....1T<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
Axion clumps with masses below the stellar range, known as Axion Bose Clusters or “miniclus- ters”, have been considered as FRB progenitors. In the strong magnetic field of a compact object, an instability may arise in a minicluster, causing it to explosively decay into photons via a synchrotron maser mechanism.<br />
<br />
== Observational Constraints ==<br />
<br />
To be filled in with updated draft</div>Apwhttps://frbtheorycat.org/index.php?title=Axion_Cloud_and_BH&diff=200Axion Cloud and BH2018-10-10T09:12:07Z<p>Apw: </p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Collision / Interaction<br />
|Progenitor = Superradiant Axion Cloud and BH<br />
|Type = Repeat<br />
|EnergyMechanism = Laser<br />
|EmissionMechanism = Synch.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = Yes<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/pdf/1709.06581.pdf<br />
|Comments = Observational counterparts could be associated with electron-positron annihilation and/or positronium.<br />
}}<br />
<br />
== Model Description ==<br />
<br />
Spinning BHs have superradiant instabilities, and thus may be surrounded by a dense superradiant axion cloud. Similarly to how a laser can be generated by stimulated axion decay in dense axion clusters, a laser can be triggered in superradiant axion clusters. Such is known as a black hole laser powered by axion superradiant instabilities (BLAST). For a BLAST’s emission to be consistent with FRB observations, the required mass dictates that the BHs be primordial. However, because PBHs form when over densities of gas collapse, they do not have spin, and are unlikely to spin up via accretion. The merging of two PBHs is thus considered for FRBs, where the required spin and resultant superradiant instabilities can be induced. Repeating bursts could occur: the BLAST will form a photon plasma that blocks axion decay and thus halts lasing until e+/e− annihilation reduces the plasma density, and the process can restart. <br />
<br />
== Observational Constraints ==<br />
<br />
Observational counterparts could be associated with e+e− annihilation and/or positronium (a bound particle of an e+ and e−), though these are not specified. GWs are also expected.</div>Apwhttps://frbtheorycat.org/index.php?title=Annihilating_Mini_BHs&diff=198Annihilating Mini BHs2018-10-09T12:59:22Z<p>Apw: /* Observational Constraints */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Void<br />
|Progenitor = Annihilating Mini BHs<br />
|Type = Single<br />
|EnergyMechanism = -<br />
|EmissionMechanism = -<br />
|LFRadioCounterpart = -<br />
|HFRadioCounterpart = - <br />
|MicrowaveCounterpart = -<br />
|THzCounterpart = -<br />
|OIRCounterpart = -<br />
|XrayCounterpart = -<br />
|GammarayCounterpart = -<br />
|GWCounterpart = -<br />
|NeutrinoCounterpart = -<br />
|References = https://arxiv.org/pdf/1206.4135.pdf<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
When a BH evaporates to some critical mass, a fireball of e+/e− pairs can be created. The relativistic pairs expand into the magnetic field of the surrounding ISM, which, for a sufficiently low mass BH, could produce a emission consistent with an FRB.<br />
<br />
== Observational Constraints ==<br />
<br />
In this scenario the inferred distance to the Lorimer burst is calculated to be <= 20 kpc, putting the source within out Galaxy. This theory is considered inviable.</div>Apwhttps://frbtheorycat.org/index.php?title=Annihilating_Mini_BHs&diff=197Annihilating Mini BHs2018-10-09T12:16:15Z<p>Apw: /* Model Description */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Void<br />
|Progenitor = Annihilating Mini BHs<br />
|Type = Single<br />
|EnergyMechanism = -<br />
|EmissionMechanism = -<br />
|LFRadioCounterpart = -<br />
|HFRadioCounterpart = - <br />
|MicrowaveCounterpart = -<br />
|THzCounterpart = -<br />
|OIRCounterpart = -<br />
|XrayCounterpart = -<br />
|GammarayCounterpart = -<br />
|GWCounterpart = -<br />
|NeutrinoCounterpart = -<br />
|References = https://arxiv.org/pdf/1206.4135.pdf<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
When a BH evaporates to some critical mass, a fireball of e+/e− pairs can be created. The relativistic pairs expand into the magnetic field of the surrounding ISM, which, for a sufficiently low mass BH, could produce a emission consistent with an FRB.<br />
<br />
== Observational Constraints ==<br />
<br />
In this scenario the inferred distance to the Lorimer burst is calculated to be 200 kpc -- far too low, thus making this theory inviable.</div>Apwhttps://frbtheorycat.org/index.php?title=Annihilating_Mini_BHs&diff=196Annihilating Mini BHs2018-10-09T12:14:12Z<p>Apw: /* Observational Constraints */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Void<br />
|Progenitor = Annihilating Mini BHs<br />
|Type = Single<br />
|EnergyMechanism = -<br />
|EmissionMechanism = -<br />
|LFRadioCounterpart = -<br />
|HFRadioCounterpart = - <br />
|MicrowaveCounterpart = -<br />
|THzCounterpart = -<br />
|OIRCounterpart = -<br />
|XrayCounterpart = -<br />
|GammarayCounterpart = -<br />
|GWCounterpart = -<br />
|NeutrinoCounterpart = -<br />
|References = https://arxiv.org/pdf/1206.4135.pdf<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
When a BH evaporates to some critical mass, a fireball of e+− pairs can be created. The relativistic pairs expand into the magnetic field of the surrounding ISM, which, for a sufficiently low mass BH, could produce a emission consistent with an FRB.<br />
<br />
== Observational Constraints ==<br />
<br />
In this scenario the inferred distance to the Lorimer burst is calculated to be 200 kpc -- far too low, thus making this theory inviable.</div>Apwhttps://frbtheorycat.org/index.php?title=Annihilating_Mini_BHs&diff=195Annihilating Mini BHs2018-10-09T12:13:26Z<p>Apw: </p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Void<br />
|Progenitor = Annihilating Mini BHs<br />
|Type = Single<br />
|EnergyMechanism = -<br />
|EmissionMechanism = -<br />
|LFRadioCounterpart = -<br />
|HFRadioCounterpart = - <br />
|MicrowaveCounterpart = -<br />
|THzCounterpart = -<br />
|OIRCounterpart = -<br />
|XrayCounterpart = -<br />
|GammarayCounterpart = -<br />
|GWCounterpart = -<br />
|NeutrinoCounterpart = -<br />
|References = https://arxiv.org/pdf/1206.4135.pdf<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
When a BH evaporates to some critical mass, a fireball of e+− pairs can be created. The relativistic pairs expand into the magnetic field of the surrounding ISM, which, for a sufficiently low mass BH, could produce a emission consistent with an FRB.<br />
<br />
== Observational Constraints ==<br />
<br />
In this scenario the inferred distance to the Lorimer burst is calculated to be 200 kpc -- far too little, thus making this theory inviable.</div>Apwhttps://frbtheorycat.org/index.php?title=Annihilating_Mini_BHs&diff=194Annihilating Mini BHs2018-10-09T12:12:46Z<p>Apw: </p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Void<br />
|Progenitor = Annihilating Mini BHs<br />
|Type = Single<br />
|EnergyMechanism = N/A<br />
|EmissionMechanism = N/A<br />
|LFRadioCounterpart = N/A<br />
|HFRadioCounterpart = N/A <br />
|MicrowaveCounterpart = N/A<br />
|THzCounterpart = N/A<br />
|OIRCounterpart = N/A<br />
|XrayCounterpart = N/A<br />
|GammarayCounterpart = N/A<br />
|GWCounterpart = N/A<br />
|NeutrinoCounterpart = N/A<br />
|References = https://arxiv.org/pdf/1206.4135.pdf<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
When a BH evaporates to some critical mass, a fireball of e+− pairs can be created. The relativistic pairs expand into the magnetic field of the surrounding ISM, which, for a sufficiently low mass BH, could produce a emission consistent with an FRB.<br />
<br />
== Observational Constraints ==<br />
<br />
In this scenario the inferred distance to the Lorimer burst is calculated to be 200 kpc -- far too little, thus making this theory inviable.</div>Apwhttps://frbtheorycat.org/index.php?title=Annihilating_Mini_BHs&diff=193Annihilating Mini BHs2018-10-09T12:10:53Z<p>Apw: /* Model Description */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Void<br />
|Progenitor = Annihilating Mini BHs<br />
|Type = Single<br />
|EnergyMechanism = N/A<br />
|EmissionMechanism = N/A<br />
|LFRadioCounterpart = N/A<br />
|HFRadioCounterpart = N/A <br />
|MicrowaveCounterpart = N/A<br />
|THzCounterpart = N/A<br />
|OIRCounterpart = N/A<br />
|XrayCounterpart = N/A<br />
|GammarayCounterpart = N/A<br />
|GWCounterpart = N/A<br />
|NeutrinoCounterpart = N/A<br />
|References = https://arxiv.org/pdf/1206.4135.pdf<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
When a BH evaporates to some critical mass, a fireball of e+− pairs can be created. The relativistic pairs expand into the magnetic field of the surrounding ISM, which, for a sufficiently low mass BH, could produce a emission consistent with an FRB.<br />
<br />
== Observational Constraints ==<br />
<br />
N/A</div>Apwhttps://frbtheorycat.org/index.php?title=WD-BH_Merger&diff=192WD-BH Merger2018-10-09T11:29:44Z<p>Apw: </p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Merger<br />
|Progenitor = WD-BH<br />
|Type = Single<br />
|EnergyMechanism = Maser<br />
|EmissionMechanism = Synch.<br />
|LFRadioCounterpart = --<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = Yes (transient accretion disk)<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2018RAA....18...61L<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
--To fill in with updated draft--<br />
<br />
== Observational Constraints ==<br />
<br />
--</div>Apwhttps://frbtheorycat.org/index.php?title=WD-BH_Merger&diff=191WD-BH Merger2018-10-09T11:28:52Z<p>Apw: </p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Merger<br />
|Progenitor = WD-BH<br />
|Type = Single<br />
|EnergyMechanism = Maser<br />
|EmissionMechanism = Synch.<br />
|LFRadioCounterpart = --<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = Yes (from transient accretion disk)<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2018RAA....18...61L<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
--To fill in with updated draft--<br />
<br />
== Observational Constraints ==<br />
<br />
--</div>Apwhttps://frbtheorycat.org/index.php?title=WD-WD_Merger&diff=190WD-WD Merger2018-10-09T11:26:42Z<p>Apw: </p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Merger<br />
|Progenitor = WD-WD <br />
|Type = Single<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes <br />
|HFRadioCounterpart = --<br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = Supernova<br />
|XrayCounterpart = Afterglow<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2013ApJ...776L..39K<br />
|Comments = --<br />
}}<br />
<br />
== Model Description ==<br />
It has been proposed that FRBs may form when a doubly-degenerate binary WD merger forms a rapidly rotating, magnetized, massive WD. The rapid rotation of the WD merger transports, via convection, inner magnetic fields to the polar regions, which greatly enhances the magnetic field strength. In the polar regions, where the magnetic fields are twisted by differential rotation or magnetic instabilities, reconnection is triggered, and electron bunches are injected into the polar region in a timescale comparable with FRBs. The electrons are accelerated to relativistic speeds along magnetic field lines, creating curvature radiation. WDs transfer angular momentum into the surrounding debris disk, rapidly reducing their rotation speed and hampering multiple FRB events.<br />
<br />
== Observational Constraints ==<br />
The event rate of such a scenario is consistent with that predicted for FRBs.</div>Apwhttps://frbtheorycat.org/index.php?title=WD-WD_Merger&diff=189WD-WD Merger2018-10-09T11:25:46Z<p>Apw: /* Observational Constraints */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Merger<br />
|Progenitor = WD-WD <br />
|Type = Single<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes <br />
|HFRadioCounterpart = --<br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = Supernova<br />
|XrayCounterpart = Afterglow<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2013ApJ...776L..39K<br />
|Comments = --<br />
}}<br />
<br />
== Model Description ==<br />
It has been proposed that FRBs may form when a doubly-degenerate binary WD merger forms a rapidly rotating, magnetized, massive WD. The rapid rotation of the WD merger transports, via convection, inner magnetic fields to the polar regions, which greatly enhances the magnetic field strength. In the polar regions, where the magnetic fields are twisted by differential rotation or magnetic instabilities, reconnection is triggered, and electron bunches are injected into the polar region in a timescale comparable with FRBs. The electrons are accelerated to relativistic speeds along magnetic field lines, creating curvature radiation. WDs transfer angular momentum into the surrounding debris disk, rapidly reducing their rotation speed and hampering multiple FRB events.<br />
<br />
== Observational Constraints ==<br />
The event rate of such a scenario is consistent with that predicted for FRBs. Whether FRBs can penetrate SN ejecta has, however, been called into question.</div>Apwhttps://frbtheorycat.org/index.php?title=WD-WD_Merger&diff=188WD-WD Merger2018-10-09T11:24:41Z<p>Apw: /* Model Description */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Merger<br />
|Progenitor = WD-WD <br />
|Type = Single<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes <br />
|HFRadioCounterpart = --<br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = Supernova<br />
|XrayCounterpart = Afterglow<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2013ApJ...776L..39K<br />
|Comments = --<br />
}}<br />
<br />
== Model Description ==<br />
It has been proposed that FRBs may form when a doubly-degenerate binary WD merger forms a rapidly rotating, magnetized, massive WD. The rapid rotation of the WD merger transports, via convection, inner magnetic fields to the polar regions, which greatly enhances the magnetic field strength. In the polar regions, where the magnetic fields are twisted by differential rotation or magnetic instabilities, reconnection is triggered, and electron bunches are injected into the polar region in a timescale comparable with FRBs. The electrons are accelerated to relativistic speeds along magnetic field lines, creating curvature radiation. WDs transfer angular momentum into the surrounding debris disk, rapidly reducing their rotation speed and hampering multiple FRB events.<br />
<br />
== Observational Constraints ==<br />
The event rate of such a scenario is consistent with that predicted for FRBs.</div>Apwhttps://frbtheorycat.org/index.php?title=WD-WD_Merger&diff=187WD-WD Merger2018-10-09T11:24:07Z<p>Apw: </p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Merger<br />
|Progenitor = WD-WD <br />
|Type = Single<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes <br />
|HFRadioCounterpart = --<br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = Supernova<br />
|XrayCounterpart = Afterglow<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2013ApJ...776L..39K<br />
|Comments = --<br />
}}<br />
<br />
== Model Description ==<br />
--this needs to be finished--<br />
It has been proposed that FRBs may form when a doubly-degenerate binary WD merger forms a rapidly rotating, magnetized, massive WD. The rapid rotation of the WD merger transports, via convection, inner magnetic fields to the polar regions, which greatly enhances the magnetic field strength. In the polar regions, where the magnetic fields are twisted by differential rotation or magnetic instabilities, reconnection is triggered, and electron bunches are injected into the polar region in a timescale comparable with FRBs. The electrons are accelerated to relativistic speeds along magnetic field lines, creating curvature radiation. WDs transfer angular momentum into the surrounding debris disk, rapidly reducing their rotation speed and hampering multiple FRB events.<br />
<br />
== Observational Constraints ==<br />
The event rate of such a scenario is consistent with that predicted for FRBs.</div>Apwhttps://frbtheorycat.org/index.php?title=WD-WD_Merger&diff=186WD-WD Merger2018-10-09T11:23:16Z<p>Apw: /* Model Description */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Merger<br />
|Progenitor = WD-WD <br />
|Type = Single<br />
|EnergyMechanism = Mag. reconnection<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes <br />
|HFRadioCounterpart = --<br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = Supernova<br />
|XrayCounterpart = Afterglow<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2013ApJ...776L..39K<br />
|Comments = --<br />
}}<br />
<br />
== Model Description ==<br />
--this needs to be finished--<br />
It has been proposed that FRBs may form when a doubly-degenerate binary WD merger forms a rapidly rotating, magnetized, massive WD. The rapid rotation of the WD merger transports, via convection, inner magnetic fields to the polar regions, which greatly enhances the magnetic field strength. In the polar regions, where the magnetic fields are twisted by differential rotation or magnetic instabilities, reconnection is triggered, and electron bunches are injected into the polar region in a timescale comparable with FRBs. The electrons are accelerated to relativistic speeds along magnetic field lines, creating curvature radiation. WDs transfer angular momentum into the surrounding debris disk, rapidly reducing their rotation speed and hampering multiple FRB events.</div>Apwhttps://frbtheorycat.org/index.php?title=Wandering_Pulsar&diff=185Wandering Pulsar2018-10-09T11:12:12Z<p>Apw: /* Observational Constraints */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Other<br />
|Progenitor = Wandering Pulsar Beams<br />
|Type = Repeat<br />
|EnergyMechanism = --<br />
|EmissionMechanism = --<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/pdf/1611.01243.pdf<br />
|Comments = Any counterparts will be associated with the pulsar, but are not specified.<br />
}}<br />
<br />
== Model Description ==<br />
<br />
This model assumes the presence of a steady beam of pulsar emission whose directly randomly changes. If this beam sweeps across the line of sight of an observer, it may be observable as an FRB. The duration of the FRB depends on the speed at which the beam moves across the sky, and hence a wandering beam mitigates the enormous power and high spin-down requirements of giant pulse and flare models.<br />
<br />
== Observational Constraints ==<br />
<br />
This scenario can also consistently explain two pairs of possibly distinct radio bursts detected in FRB 121102. Details about an emission mechanism or possible counterparts are not given.</div>Apwhttps://frbtheorycat.org/index.php?title=Wandering_Pulsar&diff=184Wandering Pulsar2018-10-09T11:09:42Z<p>Apw: /* Model Description */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Other<br />
|Progenitor = Wandering Pulsar Beams<br />
|Type = Repeat<br />
|EnergyMechanism = --<br />
|EmissionMechanism = --<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = https://arxiv.org/pdf/1611.01243.pdf<br />
|Comments = Any counterparts will be associated with the pulsar, but are not specified.<br />
}}<br />
<br />
== Model Description ==<br />
<br />
This model assumes the presence of a steady beam of pulsar emission whose directly randomly changes. If this beam sweeps across the line of sight of an observer, it may be observable as an FRB. The duration of the FRB depends on the speed at which the beam moves across the sky, and hence a wandering beam mitigates the enormous power and high spin-down requirements of giant pulse and flare models.<br />
<br />
== Observational Constraints ==<br />
<br />
To be filled in with updated draft</div>Apwhttps://frbtheorycat.org/index.php?title=Pulsar_Lightning&diff=183Pulsar Lightning2018-10-09T11:02:58Z<p>Apw: /* Observational Constraints */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Other<br />
|Progenitor = Pulsar Lightning<br />
|Type = Repeat<br />
|EnergyMechanism = Electrostatic<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2017MNRAS.469L..39K<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
Akin to SGRs powered by the release magnetic energy stored in magnetars, FRBs may be powered by the release of electrostatic energy stored in pulsars. Provided there are regions of magnetospheric plasma with distinct energy, separated by a vacuum gap, the discharge of such energy could manifest as “pulsar lighting”, analogous to the flow of current in the atmosphere when lightning strikes. This intense, rapidly varying, electric field in the gaps would accelerate electrons and positrons in the magnetosphere, producing coherent curvature radiation observable as an FRB.<br />
<br />
== Observational Constraints ==<br />
<br />
The large variation of FRB 121102 burst widths, and hence the variation of spectra fluences and frequencies, are consistent with this model.</div>Apwhttps://frbtheorycat.org/index.php?title=Pulsar_Lightning&diff=182Pulsar Lightning2018-10-09T11:01:43Z<p>Apw: /* Model Description */</p>
<hr />
<div><br />
<br />
<!-- Brings in the summary table --><br />
<!-- This is an example. Change the right hand side of all these assignments --><br />
{{FRBTableTemplate<br />
|Category = Other<br />
|Progenitor = Pulsar Lightning<br />
|Type = Repeat<br />
|EnergyMechanism = Electrostatic<br />
|EmissionMechanism = Curv.<br />
|LFRadioCounterpart = Yes<br />
|HFRadioCounterpart = -- <br />
|MicrowaveCounterpart = --<br />
|THzCounterpart = --<br />
|OIRCounterpart = --<br />
|XrayCounterpart = --<br />
|GammarayCounterpart = --<br />
|GWCounterpart = --<br />
|NeutrinoCounterpart = --<br />
|References = http://adsabs.harvard.edu/abs/2017MNRAS.469L..39K<br />
|Comments = None<br />
}}<br />
<br />
== Model Description ==<br />
<br />
Akin to SGRs powered by the release magnetic energy stored in magnetars, FRBs may be powered by the release of electrostatic energy stored in pulsars. Provided there are regions of magnetospheric plasma with distinct energy, separated by a vacuum gap, the discharge of such energy could manifest as “pulsar lighting”, analogous to the flow of current in the atmosphere when lightning strikes. This intense, rapidly varying, electric field in the gaps would accelerate electrons and positrons in the magnetosphere, producing coherent curvature radiation observable as an FRB.<br />
<br />
== Observational Constraints ==<br />
<br />
To be filled in with updated draft</div>Apw