White Holes: Difference between revisions

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== Model Description ==
== Model Description ==


To be filled in with updated draft
Should a collapsing star reach the Planck density---to become 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 and Gamma-rays characterized by the material expelled in the explosion .


== Observational Constraints ==
== Observational Constraints ==


To be filled in with updated draft
To be filled in with updated draft

Revision as of 05:39, 11 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
Other White Holes Single -- -- Yes -- -- -- Yes -- Yes -- -- http://adsabs.harvard.edu/abs/2014PhRvD..90l7503B, https://arxiv.org/pdf/1801.03841.pdf 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---to become 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 and Gamma-rays characterized by the material expelled in the explosion .

Observational Constraints

To be filled in with updated draft