NS and Asteroid Belt: Difference between revisions
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|GWCounterpart = -- | |GWCounterpart = -- | ||
|NeutrinoCounterpart = -- | |NeutrinoCounterpart = -- | ||
|References = http://adsabs.harvard.edu/abs/2016ApJ...829...27D | |References = http://adsabs.harvard.edu/abs/2016ApJ...829...27D, http://iopscience.iop.org/article/10.3847/2041-8213/aa65c9/pdf | ||
|Comments = None | |Comments = None | ||
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Latest revision as of 11:43, 16 October 2018
| 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.