Tiny EM Explosions - Revision history

Shriharsh at 23:47, 12 October 2018

2018-10-12T23:47:19Z

← Older revision		Revision as of 19:47, 12 October 2018
Line 18:		Line 18:
	\|GWCounterpart = --		\|GWCounterpart = --
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2017ApJ...844..162T , http://adsabs.harvard.edu/abs/2017ApJ...844...65T		\|References = http://adsabs.harvard.edu/abs/2017ApJ...844..162T, http://adsabs.harvard.edu/abs/2017ApJ...844...65T
	\|Comments = None		\|Comments = None
	}}		}}

Shriharsh at 23:47, 12 October 2018

2018-10-12T23:47:02Z

← Older revision		Revision as of 19:47, 12 October 2018
Line 18:		Line 18:
	\|GWCounterpart = --		\|GWCounterpart = --
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2017ApJ...844..162T,http://adsabs.harvard.edu/abs/2017ApJ...844...65T		\|References = http://adsabs.harvard.edu/abs/2017ApJ...844..162T , http://adsabs.harvard.edu/abs/2017ApJ...844...65T
	\|Comments = None		\|Comments = None
	}}		}}

Shriharsh at 23:46, 12 October 2018

2018-10-12T23:46:35Z

← Older revision		Revision as of 19:46, 12 October 2018
Line 18:		Line 18:
	\|GWCounterpart = --		\|GWCounterpart = --
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/~~cgi-bin~~/~~bib_query?arXiv:1703~~.~~00393~~, http://adsabs.harvard.edu/abs/2017ApJ...844...65T		\|References = http://adsabs.harvard.edu/abs/2017ApJ...844..162T,http://adsabs.harvard.edu/abs/2017ApJ...844...65T
	\|Comments = None		\|Comments = None
	}}		}}

Jake Gordin: /* Observational Constraints */

2018-10-11T11:30:48Z

Observational Constraints

← Older revision		Revision as of 07:30, 11 October 2018
Line 31:		Line 31:
	== Observational Constraints ==		== Observational Constraints ==

	~~To be filled in with updated draft~~		--

Sulona: /* Model Description */

2018-10-11T10:15:38Z

Model Description

← Older revision		Revision as of 06:15, 11 October 2018
Line 27:		Line 27:
	The collision of two relativistic macroscopic dipoles that form around the time of cosmic electroweak symmetry-breaking could cause a tiny explosion. Tiny electromagnetic explosions occur when the initial wavelength of the explosion is narrower than the wavelength of the radiation observed so the energy travels outwards in a very thin shell, and the surrounding charged particles are deflected (as opposed to reflected) by the magnetic field embedded in the expanding shell.		The collision of two relativistic macroscopic dipoles that form around the time of cosmic electroweak symmetry-breaking could cause a tiny explosion. Tiny electromagnetic explosions occur when the initial wavelength of the explosion is narrower than the wavelength of the radiation observed so the energy travels outwards in a very thin shell, and the surrounding charged particles are deflected (as opposed to reflected) by the magnetic field embedded in the expanding shell.

	To retain the supporting electric field for cosmological timescales, these field structures must be superconducting, and are thus dubbed large superconducting dipoles (LSD) - the term "Large" is relative, and is used because the dipoles are macroscopic. The expanding relativistic magnetized shell from the explosion couples efficiently to a low-frequency, strong, superluminal EM wave in the surrounding plasma, allowing the emission to escape. Three emission mechanisms are possible: the reflection of an ambient static magnetic field by the conducting surface of the shell; direct linear conversion of the magnetic field in the shell; and the excitation of an EM wave if the surface of the shell becomes corrugated via the reconnection of the ejected magnetic field with the ambient magnetic field. The deceleration of the magnetic shell causes a higher frequency radio pulse and the thermal part of the explosion radiates ~~\gamma~~-rays, however the latter are not expected to be detectable. The model accounts for repeating and non-repeating FRBs and for their observed differences in linear polarizations and RMs - the hydromagnetic drag on LSDs is weak in the ISM, and strong in high - density environments. As such, a slowly accreting SMBH may capture LSDs and group them in gravitationally bound cusps, within which the LSDs collide and create repeating FRBs. Here the high density plasma accounts for the high linear polarization and high RM observed in FRB 121102. The opposite is true for LSDs far from the SMBH; where the observed RM is low and signals are non-repeating, such as in FRB 150215, collisions are expected to take place in dark matter halos of galaxies.		To retain the supporting electric field for cosmological timescales, these field structures must be superconducting, and are thus dubbed large superconducting dipoles (LSD) - the term "Large" is relative, and is used because the dipoles are macroscopic. The expanding relativistic magnetized shell from the explosion couples efficiently to a low-frequency, strong, superluminal EM wave in the surrounding plasma, allowing the emission to escape. Three emission mechanisms are possible: the reflection of an ambient static magnetic field by the conducting surface of the shell; direct linear conversion of the magnetic field in the shell; and the excitation of an EM wave if the surface of the shell becomes corrugated via the reconnection of the ejected magnetic field with the ambient magnetic field. The deceleration of the magnetic shell causes a higher frequency radio pulse and the thermal part of the explosion radiates Gamma-rays, however the latter are not expected to be detectable. The model accounts for repeating and non-repeating FRBs and for their observed differences in linear polarizations and RMs - the hydromagnetic drag on LSDs is weak in the ISM, and strong in high - density environments. As such, a slowly accreting SMBH may capture LSDs and group them in gravitationally bound cusps, within which the LSDs collide and create repeating FRBs. Here the high density plasma accounts for the high linear polarization and high RM observed in FRB 121102. The opposite is true for LSDs far from the SMBH; where the observed RM is low and signals are non-repeating, such as in FRB 150215, collisions are expected to take place in dark matter halos of galaxies.

	== Observational Constraints ==		== Observational Constraints ==

	To be filled in with updated draft		To be filled in with updated draft

Sulona: /* Model Description */

2018-10-11T10:15:11Z

Model Description

← Older revision		Revision as of 06:15, 11 October 2018
Line 27:		Line 27:
	The collision of two relativistic macroscopic dipoles that form around the time of cosmic electroweak symmetry-breaking could cause a tiny explosion. Tiny electromagnetic explosions occur when the initial wavelength of the explosion is narrower than the wavelength of the radiation observed so the energy travels outwards in a very thin shell, and the surrounding charged particles are deflected (as opposed to reflected) by the magnetic field embedded in the expanding shell.		The collision of two relativistic macroscopic dipoles that form around the time of cosmic electroweak symmetry-breaking could cause a tiny explosion. Tiny electromagnetic explosions occur when the initial wavelength of the explosion is narrower than the wavelength of the radiation observed so the energy travels outwards in a very thin shell, and the surrounding charged particles are deflected (as opposed to reflected) by the magnetic field embedded in the expanding shell.

	To retain the supporting electric field for cosmological timescales, these field structures must be superconducting, and are thus dubbed large superconducting dipoles (LSD) - the term "Large" is relative, and is used because the dipoles are macroscopic. The expanding relativistic magnetized shell from the explosion couples efficiently to a low-frequency, strong, superluminal EM wave in the surrounding plasma, allowing the emission to escape. Three emission mechanisms are possible: the reflection of an ambient static magnetic field by the conducting surface of the shell; direct linear conversion of the magnetic field in the shell; and the excitation of an EM wave if the surface of the shell becomes corrugated via the reconnection of the ejected magnetic field with the ambient magnetic field. The deceleration of the magnetic shell causes a higher frequency radio pulse and the thermal part of the explosion radiates $\gamma$-rays, however the latter are not expected to be detectable. The model accounts for repeating and non-repeating FRBs and for their observed differences in linear polarizations and RMs - the hydromagnetic drag on LSDs is weak in the ISM, and strong in high - density environments. As such, a slowly accreting SMBH may capture LSDs and group them in gravitationally bound cusps, within which the LSDs collide and create repeating FRBs. Here the high density plasma accounts for the high linear polarization and high RM observed in FRB 121102. The opposite is true for LSDs far from the SMBH; where the observed RM is low and signals are non-repeating, such as in FRB 150215, collisions are expected to take place in dark matter halos of galaxies.		To retain the supporting electric field for cosmological timescales, these field structures must be superconducting, and are thus dubbed large superconducting dipoles (LSD) - the term "Large" is relative, and is used because the dipoles are macroscopic. The expanding relativistic magnetized shell from the explosion couples efficiently to a low-frequency, strong, superluminal EM wave in the surrounding plasma, allowing the emission to escape. Three emission mechanisms are possible: the reflection of an ambient static magnetic field by the conducting surface of the shell; direct linear conversion of the magnetic field in the shell; and the excitation of an EM wave if the surface of the shell becomes corrugated via the reconnection of the ejected magnetic field with the ambient magnetic field. The deceleration of the magnetic shell causes a higher frequency radio pulse and the thermal part of the explosion radiates \gamma-rays, however the latter are not expected to be detectable. The model accounts for repeating and non-repeating FRBs and for their observed differences in linear polarizations and RMs - the hydromagnetic drag on LSDs is weak in the ISM, and strong in high - density environments. As such, a slowly accreting SMBH may capture LSDs and group them in gravitationally bound cusps, within which the LSDs collide and create repeating FRBs. Here the high density plasma accounts for the high linear polarization and high RM observed in FRB 121102. The opposite is true for LSDs far from the SMBH; where the observed RM is low and signals are non-repeating, such as in FRB 150215, collisions are expected to take place in dark matter halos of galaxies.

	== Observational Constraints ==		== Observational Constraints ==

	To be filled in with updated draft		To be filled in with updated draft

Sulona: /* Model Description */

2018-10-11T10:14:42Z

Model Description

← Older revision		Revision as of 06:14, 11 October 2018
Line 27:		Line 27:
	The collision of two relativistic macroscopic dipoles that form around the time of cosmic electroweak symmetry-breaking could cause a tiny explosion. Tiny electromagnetic explosions occur when the initial wavelength of the explosion is narrower than the wavelength of the radiation observed so the energy travels outwards in a very thin shell, and the surrounding charged particles are deflected (as opposed to reflected) by the magnetic field embedded in the expanding shell.		The collision of two relativistic macroscopic dipoles that form around the time of cosmic electroweak symmetry-breaking could cause a tiny explosion. Tiny electromagnetic explosions occur when the initial wavelength of the explosion is narrower than the wavelength of the radiation observed so the energy travels outwards in a very thin shell, and the surrounding charged particles are deflected (as opposed to reflected) by the magnetic field embedded in the expanding shell.

	To retain the supporting electric field for cosmological timescales, these field structures must be superconducting, and are thus dubbed large superconducting dipoles (LSD) - the term ``Large'' is relative, and is used because the dipoles are macroscopic. The expanding relativistic magnetized shell from the explosion couples efficiently to a low-frequency, strong, superluminal EM wave in the surrounding plasma, allowing the emission to escape. Three emission mechanisms are possible: the reflection of an ambient static magnetic field by the conducting surface of the shell; direct linear conversion of the magnetic field in the shell; and the excitation of an EM wave if the surface of the shell becomes corrugated via the reconnection of the ejected magnetic field with the ambient magnetic field. The deceleration of the magnetic shell causes a higher frequency radio pulse and the thermal part of the explosion radiates $\gamma$-rays, however the latter are not expected to be detectable. The model accounts for repeating and non-repeating FRBs and for their observed differences in linear polarizations and RMs - the hydromagnetic drag on LSDs is weak in the ISM, and strong in high - density environments. As such, a slowly accreting SMBH may capture LSDs and group them in gravitationally bound cusps, within which the LSDs collide and create repeating FRBs. Here the high density plasma accounts for the high linear polarization and high RM observed in FRB 121102. The opposite is true for LSDs far from the SMBH; where the observed RM is low and signals are non-repeating, such as in FRB 150215, collisions are expected to take place in dark matter halos of galaxies.		To retain the supporting electric field for cosmological timescales, these field structures must be superconducting, and are thus dubbed large superconducting dipoles (LSD) - the term "Large" is relative, and is used because the dipoles are macroscopic. The expanding relativistic magnetized shell from the explosion couples efficiently to a low-frequency, strong, superluminal EM wave in the surrounding plasma, allowing the emission to escape. Three emission mechanisms are possible: the reflection of an ambient static magnetic field by the conducting surface of the shell; direct linear conversion of the magnetic field in the shell; and the excitation of an EM wave if the surface of the shell becomes corrugated via the reconnection of the ejected magnetic field with the ambient magnetic field. The deceleration of the magnetic shell causes a higher frequency radio pulse and the thermal part of the explosion radiates $\gamma$-rays, however the latter are not expected to be detectable. The model accounts for repeating and non-repeating FRBs and for their observed differences in linear polarizations and RMs - the hydromagnetic drag on LSDs is weak in the ISM, and strong in high - density environments. As such, a slowly accreting SMBH may capture LSDs and group them in gravitationally bound cusps, within which the LSDs collide and create repeating FRBs. Here the high density plasma accounts for the high linear polarization and high RM observed in FRB 121102. The opposite is true for LSDs far from the SMBH; where the observed RM is low and signals are non-repeating, such as in FRB 150215, collisions are expected to take place in dark matter halos of galaxies.

	== Observational Constraints ==		== Observational Constraints ==

	To be filled in with updated draft		To be filled in with updated draft

Sulona: /* Model Description */

2018-10-11T10:14:01Z

Model Description

← Older revision		Revision as of 06:14, 11 October 2018
Line 24:		Line 24:
	== Model Description ==		== Model Description ==

	To be ~~filled~~ in with ~~updated draft~~
			The collision of two relativistic macroscopic dipoles that form around the time of cosmic electroweak symmetry-breaking could cause a tiny explosion. Tiny electromagnetic explosions occur when the initial wavelength of the explosion is narrower than the wavelength of the radiation observed so the energy travels outwards in a very thin shell, and the surrounding charged particles are deflected (as opposed to reflected) by the magnetic field embedded in the expanding shell.

			To retain the supporting electric field for cosmological timescales, these field structures must be superconducting, and are thus dubbed large superconducting dipoles (LSD) - the term ``Large'' is relative, and is used because the dipoles are macroscopic. The expanding relativistic magnetized shell from the explosion couples efficiently to a low-frequency, strong, superluminal EM wave in the surrounding plasma, allowing the emission to escape. Three emission mechanisms are possible: the reflection of an ambient static magnetic field by the conducting surface of the shell; direct linear conversion of the magnetic field in the shell; and the excitation of an EM wave if the surface of the shell becomes corrugated via the reconnection of the ejected magnetic field with the ambient magnetic field. The deceleration of the magnetic shell causes a higher frequency radio pulse and the thermal part of the explosion radiates $\gamma$-rays, however the latter are not expected to be detectable. The model accounts for repeating and non-repeating FRBs and for their observed differences in linear polarizations and RMs - the hydromagnetic drag on LSDs is weak in the ISM, and strong in high - density environments. As such, a slowly accreting SMBH may capture LSDs and group them in gravitationally bound cusps, within which the LSDs collide and create repeating FRBs. Here the high density plasma accounts for the high linear polarization and high RM observed in FRB 121102. The opposite is true for LSDs far from the SMBH; where the observed RM is low and signals are non-repeating, such as in FRB 150215, collisions are expected to take place in dark matter halos of galaxies.

	== Observational Constraints ==		== Observational Constraints ==

	To be filled in with updated draft		To be filled in with updated draft

Jake Gordin at 10:02, 11 October 2018

2018-10-11T10:02:12Z

← Older revision		Revision as of 06:02, 11 October 2018
Line 18:		Line 18:
	\|GWCounterpart = --		\|GWCounterpart = --
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = ~~https~~://~~arxiv~~.~~org~~/~~pdf~~/1703.00393~~.pdf~~, http://adsabs.harvard.edu/abs/2017ApJ...844...65T		\|References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1703.00393, http://adsabs.harvard.edu/abs/2017ApJ...844...65T
	\|Comments = None		\|Comments = None
	}}		}}

Emma Platts: Created page with " {{FRBTableTemplate |Category = Other |Pro..."

2018-10-02T14:11:42Z

Created page with "   {{FRBTableTemplate |Category = Other |Pro..."

New page

{{FRBTableTemplate
|Category = Other
|Progenitor = Tiny EM Explosions
|Type = Both
|EnergyMechanism = Thin shell interactions
|EmissionMechanism = Curv.
|LFRadioCounterpart = Yes
|HFRadioCounterpart = Yes
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = --
|XrayCounterpart = --
|GammarayCounterpart = Unlikely observable
|GWCounterpart = --
|NeutrinoCounterpart = --
|References = https://arxiv.org/pdf/1703.00393.pdf, http://adsabs.harvard.edu/abs/2017ApJ...844...65T
|Comments = None
}}

== Model Description ==

To be filled in with updated draft

== Observational Constraints ==

To be filled in with updated draft