RDM Stars: Difference between revisions
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|GWCounterpart = --- | |GWCounterpart = --- | ||
|NeutrinoCounterpart = --- | |NeutrinoCounterpart = --- | ||
|References = https://arxiv.org/pdf/1812.11801. | |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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== Observational Constraints == | == Observational Constraints == | ||
None. | |||
Latest revision as of 06:19, 27 November 2019
| 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.