Jet-Caviton - Revision history

Emma Platts at 11:05, 15 October 2018

2018-10-15T11:05:58Z

← Older revision		Revision as of 07:05, 15 October 2018
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	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2016PhRvD..93b3001R, http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1704.08097		\|References = http://adsabs.harvard.edu/abs/2016PhRvD..93b3001R, http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1704.08097
	\|Comments = ~~None~~		\|Comments = Persistent scintillating radio emission.
	}}		}}

Emma Platts at 09:18, 12 October 2018

2018-10-12T09:18:35Z

← Older revision		Revision as of 05:18, 12 October 2018
Line 24:		Line 24:
	== Model Description ==		== 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 ~~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.		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 ==		== 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.		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.

Jake Gordin at 10:52, 11 October 2018

2018-10-11T10:52:48Z

← Older revision		Revision as of 06:52, 11 October 2018
Line 24:		Line 24:
	== Model Description ==		== Model Description ==

	~~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. 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.		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 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.

	== Observational Constraints ==		== 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.		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.

Jake Gordin: /* Model Description */

2018-10-11T10:51:39Z

Model Description

← Older revision		Revision as of 06:51, 11 October 2018
Line 24:		Line 24:
	== Model Description ==		== Model Description ==

	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.		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. 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.


	== Observational Constraints ==		== 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.		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.

Jake Gordin at 09:36, 11 October 2018

2018-10-11T09:36:02Z

← Older revision		Revision as of 05:36, 11 October 2018
Line 18:		Line 18:
	\|GWCounterpart = Yes		\|GWCounterpart = Yes
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2016PhRvD..93b3001R, ~~https~~://~~arxiv~~.~~org~~/~~pdf~~/1704.08097~~.pdf~~		\|References = http://adsabs.harvard.edu/abs/2016PhRvD..93b3001R, http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1704.08097
	\|Comments = None		\|Comments = None
	}}		}}

Apw at 10:50, 10 October 2018

2018-10-10T10:50:47Z

← Older revision		Revision as of 06:50, 10 October 2018
Line 24:		Line 24:
	== Model Description ==		== Model Description ==

	* to be ~~added~~		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.


	== Observational Constraints ==		== 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.

Emma Platts at 13:12, 2 October 2018

2018-10-02T13:12:08Z

← Older revision		Revision as of 09:12, 2 October 2018
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	\|Category = AGN		\|Category = AGN
	\|Progenitor = Jet-Caviton Interaction		\|Progenitor = Jet-Caviton Interaction
	\|Type = ~~Single or Repeat~~		\|Type = Both
	\|EnergyMechanism = Electron scattering		\|EnergyMechanism = Electron scattering
	\|EmissionMechanism = Bremsst.		\|EmissionMechanism = Bremsst.

Emma Platts at 13:23, 27 September 2018

2018-09-27T13:23:40Z

← Older revision		Revision as of 09:23, 27 September 2018
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	\|EmissionMechanism = Bremsst.		\|EmissionMechanism = Bremsst.
	\|LFRadioCounterpart = Yes		\|LFRadioCounterpart = Yes
	\|HFRadioCounterpart = --		\|HFRadioCounterpart = Yes
	\|MicrowaveCounterpart = --		\|MicrowaveCounterpart = --
	\|THzCounterpart = --		\|THzCounterpart = --
Line 18:		Line 18:
	\|GWCounterpart = Yes		\|GWCounterpart = Yes
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2016PhRvD..93b3001R		\|References = http://adsabs.harvard.edu/abs/2016PhRvD..93b3001R, https://arxiv.org/pdf/1704.08097.pdf
	\|Comments = None		\|Comments = None
	}}		}}

Emma Platts: Created page with " {{FRBTableTemplate |Category = AGN |Proge..."

2018-09-27T13:15:19Z

Created page with "   {{FRBTableTemplate |Category = AGN |Proge..."

New page

{{FRBTableTemplate
|Category = AGN
|Progenitor = Jet-Caviton Interaction
|Type = Single or Repeat
|EnergyMechanism = Electron scattering
|EmissionMechanism = Bremsst.
|LFRadioCounterpart = Yes
|HFRadioCounterpart = --
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = --
|XrayCounterpart = --
|GammarayCounterpart = Possible GRB
|GWCounterpart = Yes
|NeutrinoCounterpart = --
|References = http://adsabs.harvard.edu/abs/2016PhRvD..93b3001R
|Comments = None
}}

== Model Description ==

* to be added

== Observational Constraints ==