Difference between revisions of "NS and Asteroid Belt"

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|References            = http://adsabs.harvard.edu/abs/2016ApJ...829...27D
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|References            = http://adsabs.harvard.edu/abs/2016ApJ...829...27D, http://iopscience.iop.org/article/10.3847/2041-8213/aa65c9/pdf
 
|Comments              = None
 
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Latest revision as of 12:43, 16 October 2018





Summary Table
Category Progenitor Type Energy Mechanism Emission Mechanism Counterparts References Brief Comments
LF Radio HF Radio Microwave Terahertz Optical/IR X-rays Gamma-rays Gravitational Waves Neutrinos
Collision/ Interaction NS and Asteroid Belt Repeat Electron stripping Curv. Yes -- -- -- -- -- Yes -- -- http://adsabs.harvard.edu/abs/2016ApJ...829...27D, http://iopscience.iop.org/article/10.3847/2041-8213/aa65c9/pdf None

Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)


Model Description

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.

Observational Constraints

The time between edge on collisions within the asteroid belt is consistent with the time between the signals of FRB 121102.