White Holes - Revision history

Emma Platts at 11:22, 27 November 2019

2019-11-27T11:22:59Z

← Older revision		Revision as of 07:22, 27 November 2019
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	\|GWCounterpart = --		\|GWCounterpart = --
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2014PhRvD..90l7503B, ~~http~~://~~adsabs~~.~~harvard.edu~~/~~cgi-bin~~/~~bib_query?arXiv:1611~~.~~01243~~		\|References = http://adsabs.harvard.edu/abs/2014PhRvD..90l7503B, https://arxiv.org/abs/1801.03841
	\|Comments = None		\|Comments = None
	}}		}}

Sulona: /* Observational Constraints */

2018-10-11T11:23:42Z

Observational Constraints

← Older revision		Revision as of 07:23, 11 October 2018
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	== Observational Constraints ==		== Observational Constraints ==
			-
	~~To be filled in with updated draft~~

Jake Gordin at 10:01, 11 October 2018

2018-10-11T10:01:09Z

← Older revision		Revision as of 06:01, 11 October 2018
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	\|GWCounterpart = --		\|GWCounterpart = --
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/abs/2014PhRvD..90l7503B, ~~https~~://~~arxiv~~.~~org~~/~~pdf~~/~~1801.03841~~.~~pdf~~		\|References = http://adsabs.harvard.edu/abs/2014PhRvD..90l7503B, http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1611.01243
	\|Comments = None		\|Comments = None
	}}		}}

Sulona: /* Model Description */

2018-10-11T09:41:57Z

Model Description

← Older revision		Revision as of 05:41, 11 October 2018
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	== Model Description ==		== 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 .		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 ==		== Observational Constraints ==

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

Sulona: /* Model Description */

2018-10-11T09:39:42Z

Model Description

← Older revision		Revision as of 05:39, 11 October 2018
Line 24:		Line 24:
	== 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

Emma Platts: Created page with " {{FRBTableTemplate |Category = Other |Pro..."

2018-10-02T14:19:26Z

Created page with "   {{FRBTableTemplate |Category = Other |Pro..."

New page

{{FRBTableTemplate
|Category = Other
|Progenitor = White Holes
|Type = Single
|EnergyMechanism = --
|EmissionMechanism = --
|LFRadioCounterpart = Yes
|HFRadioCounterpart = --
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = Yes
|XrayCounterpart = --
|GammarayCounterpart = Yes
|GWCounterpart = --
|NeutrinoCounterpart = --
|References = http://adsabs.harvard.edu/abs/2014PhRvD..90l7503B, https://arxiv.org/pdf/1801.03841.pdf
|Comments = None
}}

== Model Description ==

To be filled in with updated draft

== Observational Constraints ==

To be filled in with updated draft