NS and Asteroids/Comets - Revision history

Apw at 11:31, 10 October 2018

2018-10-10T11:31:02Z

← Older revision		Revision as of 07:31, 10 October 2018
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	\|THzCounterpart = --		\|THzCounterpart = --
	\|OIRCounterpart = --		\|OIRCounterpart = --
	\|XrayCounterpart = --		\|XrayCounterpart = Yes (probably too faint to detect)
	\|GammarayCounterpart = --		\|GammarayCounterpart = Yes (probably too faint to detect)
	\|GWCounterpart = --		\|GWCounterpart = --
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --

Apw at 11:28, 10 October 2018

2018-10-10T11:28:48Z

← Older revision		Revision as of 07:28, 10 October 2018
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	\|GWCounterpart = --		\|GWCounterpart = --
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2015ApJ...809...24G~~, https://arxiv.org/pdf/1512.06519.pdf~~		\|References = http://adsabs.harvard.edu/abs/2015ApJ...809...24G
	\|Comments = None		\|Comments = None
	}}		}}
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	== Model Description ==		== Model Description ==

	* to ~~add~~		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.

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

			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.

Emma Platts at 14:45, 27 September 2018

2018-09-27T14:45:26Z

← Older revision		Revision as of 10:45, 27 September 2018
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	<!-- This is an example. Change the right hand side of all these assignments -->		<!-- This is an example. Change the right hand side of all these assignments -->
	{{FRBTableTemplate		{{FRBTableTemplate
	\|Category = Collision/ ~~Collision~~		\|Category = Collision/ Interaction
	\|Progenitor = NS and Asteroids/ Comets		\|Progenitor = NS and Asteroids/ Comets
	\|Type = Single		\|Type = Single

Emma Platts at 14:45, 27 September 2018

2018-09-27T14:45:10Z

← Older revision		Revision as of 10:45, 27 September 2018
Line 4:		Line 4:
	<!-- This is an example. Change the right hand side of all these assignments -->		<!-- This is an example. Change the right hand side of all these assignments -->
	{{FRBTableTemplate		{{FRBTableTemplate
	\|Category = Collision		\|Category = Collision/ Collision
	\|Progenitor = NS and Asteroids/Comets		\|Progenitor = NS and Asteroids/ Comets
	\|Type = Single		\|Type = Single
	\|EnergyMechanism = Mag. reconnection		\|EnergyMechanism = Mag. reconnection

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

2018-09-27T14:39:20Z

Created page with "   {{FRBTableTemplate |Category = Collision..."

New page

{{FRBTableTemplate
|Category = Collision
|Progenitor = NS and Asteroids/Comets
|Type = Single
|EnergyMechanism = Mag. reconnection
|EmissionMechanism = Curv.
|LFRadioCounterpart = Yes
|HFRadioCounterpart = --
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = --
|XrayCounterpart = --
|GammarayCounterpart = --
|GWCounterpart = --
|NeutrinoCounterpart = --
|References = http://adsabs.harvard.edu/abs/2015ApJ...809...24G, https://arxiv.org/pdf/1512.06519.pdf
|Comments = None
}}

== Model Description ==

* to add

== Observational Constraints ==