Difference between revisions of "RDM Stars"

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|GWCounterpart          = ---
 
|GWCounterpart          = ---
 
|NeutrinoCounterpart    = ---
 
|NeutrinoCounterpart    = ---
|References            = https://arxiv.org/pdf/1812.11801.pdf
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|References            = https://arxiv.org/pdf/1812.11801, https://arxiv.org/abs/1906.09074
 
|Comments              = Repeaters are possible if multiple asteroids collide with the star
 
|Comments              = Repeaters are possible if multiple asteroids collide with the star
 
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== Model Description ==
 
== Model Description ==
  
This model considers a radial dark matter (RDM) stars - dark stars which are coupled to radial dark matter flows. These are kind of Planck star whose evolution has been halted by the pressure of dark matter flows surrounding the star. An FRB may be created when an asteroid falls onto the star: the large gravitational force in the RDM-star interior accelerates nucleons of the asteroid to extremely high energies. These collide with the core of the star, reacting with the Planck particles to create stimulated emission akin to an FRB.
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This model considers radial dark matter (RDM) stars - dark stars which are coupled to radial dark matter flows. These are kind of Planck star whose evolution has been halted by the pressure of dark matter flows surrounding the star. An FRB may be created when an asteroid falls onto the star: the large gravitational force in the RDM-star interior accelerates nucleons of the asteroid to extremely high energies. These collide with the core of the star, reacting with the Planck particles to create stimulated emission akin to an FRB.
  
 
== Observational Constraints ==
 
== Observational Constraints ==
  
The RDM stars considered in this model are assumed to be located in the centers of galaxies.
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None.

Latest revision as of 06:19, 27 November 2019





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
Other RDM Star Both Stimulated emission Synch. --- --- --- --- --- --- --- --- --- https://arxiv.org/pdf/1812.11801, https://arxiv.org/abs/1906.09074 Repeaters are possible if multiple asteroids collide with the star

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


Model Description

This model considers radial dark matter (RDM) stars - dark stars which are coupled to radial dark matter flows. These are kind of Planck star whose evolution has been halted by the pressure of dark matter flows surrounding the star. An FRB may be created when an asteroid falls onto the star: the large gravitational force in the RDM-star interior accelerates nucleons of the asteroid to extremely high energies. These collide with the core of the star, reacting with the Planck particles to create stimulated emission akin to an FRB.

Observational Constraints

None.