Young Magnetars

2019-09-06T13:24:14Z

Emma Platts:

Young Magnetars

2019-09-06T13:14:05Z

Emma Platts:

2018-10-17T09:48:29Z

Emma Platts:

{{FRBTableTemplate
|Category = Collapse
|Progenitor = NS to KNBH
|Type = Single
|EnergyMechanism = Mag. reconnection
|EmissionMechanism = Curv.
|LFRadioCounterpart = Yes
|HFRadioCounterpart = --
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = --
|XrayCounterpart = --
|GammarayCounterpart = --
|GWCounterpart = Yes
|NeutrinoCounterpart = --
|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.
}}

== 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 ==

--

NS to KNBH

2018-10-17T09:47:55Z

Emma Platts:

{{FRBTableTemplate
|Category = Collapse
|Progenitor = NS to KNBH
|Type = Single
|EnergyMechanism = Mag. reconnection
|EmissionMechanism = Curv.
|LFRadioCounterpart = Yes
|HFRadioCounterpart = --
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = --
|XrayCounterpart = --
|GammarayCounterpart = --
|GWCounterpart = Yes
|NeutrinoCounterpart = --
|References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1307.1409, http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1603.05509, http://adsabs.harvard.edu/abs/2014ApJ...780L..21Z
|Comments = Possible X-ray afterglow and a short/long GRB created in NS birth prior to the FRB.
}}

== 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 ==

--

NS and Asteroid Belt

2018-10-16T16:43:35Z

Emma Platts:

Main Page

2018-10-15T11:23:35Z

Emma Platts: /* Summary Table */

== Welcome to the FRB Theory Wiki! ==
This is a collaborative effort between theorists and astronomers to discuss and track theories and observations pertaining to fast radio bursts (FRBs). The field of FRBs is in its fairly nascent stages and theories are abound. It is getting hard to keep abreast of the latest ideas and observations. This wiki aims to do the following:
#Track published FRB theories, their predictions in different wavebands, current observational constraints, and future tests.
#Serve as a discussion board to hash out finer points of theories, possible extensions and modifications.
#Serve as a tracer of the zeitgeist and how (over the next decade or so) science converges on the answer(s).
#Publish 'state of theory' snapshots every year (with all contributors invited to be authors).

The FRB theory catalog and this wiki were first published as '''PAPER REFERENCE'''. Please cite XXX if it was of use to your work.

Email [[Special:EmailUser/Shriharsh | Shriharsh Tendulkar]] or [[Special:EmailUser/Weltman | Amanda Weltman]] if you need more help/information.

== Contributing to the Wiki ==
You are invited to contribute to the discussion by signing in/making an account (at the top right corner). This wiki is divided into the summary page, that concisely tabulates current FRB theories, and the individual theory discussion pages, where further discussion takes place. See [Instructions] for more details.

=== Rules and Guidelines ===
[[Instruction | Detailed Instructions]]

We expect a healthy and frank discussion of ideas on this wiki. As many of these ideas are fairly personal, arguments can get heated. We would like to remind users that this is public discussion forum. The basic rule to follow is the golden rule: ''Treat others (and others' ideas) the way you'd like to yourself or your ideas be treated''. Be fair and polite, using the same tone as a good referee report. Moderators may send warnings or ban users for not following this rule.

We expect that people will use their real names and email addresses in the login. The moderators may ask you to update your user information.

Follow the setup of the wiki in general --- For example, if a section requests a concise summary, please keep it short. Moderators will be going through editing and wordsmithing to keep a uniform look.

== Summary Table ==


{{#cargo_query:
tables = frbtheory
|fields = _pageName=Name, Category, Progenitor, Type, Energy_Mechanism, Emission_Mechanism, LF_Radio_Counterpart, HF_Radio_Counterpart, Microwave_Counterpart, THz_Counterpart, OIR_Counterpart, X_ray_Counterpart, Gamma_ray_Counterpart, GW_Counterpart, Neutrino_Counterpart, References, Comments
|where=_pageNamespace='Main'
|group by = _pageName
|format = table
|limit = 50
|order by = Category ASC

}}

Main Page

2018-10-15T11:23:00Z

Emma Platts: /* Summary Table */

Main Page

2018-10-15T11:22:33Z

Emma Platts: /* Summary Table */

Main Page

2018-10-15T11:21:22Z

Emma Platts: /* Summary Table */

2018-10-15T11:05:58Z

Emma Platts:

{{FRBTableTemplate
|Category = AGN
|Progenitor = Jet-Caviton Interaction
|Type = Both
|EnergyMechanism = Electron scattering
|EmissionMechanism = Bremsst.
|LFRadioCounterpart = Yes
|HFRadioCounterpart = Yes
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = --
|XrayCounterpart = --
|GammarayCounterpart = Possible GRB
|GWCounterpart = Yes
|NeutrinoCounterpart = --
|References = http://adsabs.harvard.edu/abs/2016PhRvD..93b3001R, http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1704.08097
|Comments = Persistent scintillating radio emission.
}}

== Model Description ==

A hot accretion disk forms 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. 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 electron-positron 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.

== Observational Constraints ==

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.