White Holes

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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 White Holes Single -- -- Yes -- -- -- Yes -- Yes -- -- http://adsabs.harvard.edu/abs/2014PhRvD..90l7503B, http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1611.01243 None

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


Model Description

Should a collapsing star reach the Planck density, becoming a Planck star, it will cease to collapse further and will explode outwards (or bounce) to form a white hole (WH). Due to their age, PBHs or Planck stars are the strongest candidates to form WHs which may be observable today, and the energy they release is consistent with FRBs. A single FRB is expected, accompanied by an IR signal - with a wave length on the order of the exploding star -, as well as Gamma-rays, characterized by the material expelled in the explosion .

Observational Constraints

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