Annihilating Mini BHs - Revision history

Emma Platts at 08:37, 12 October 2018

2018-10-12T08:37:38Z

← Older revision		Revision as of 04:37, 12 October 2018
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	<!-- This is an example. Change the right hand side of all these assignments -->		<!-- This is an example. Change the right hand side of all these assignments -->
	{{FRBTableTemplate		{{FRBTableTemplate
	\|Category = ~~Void~~		\|Category = Inviable
	\|Progenitor = Annihilating Mini BHs		\|Progenitor = Annihilating Mini BHs
	\|Type = Single		\|Type = Single
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	== Model Description ==		== Model Description ==

	When a BH evaporates to some critical mass, a fireball of ~~$e^+_~~-$ pairs can be created. The relativistic pairs expand into the magnetic field of the surrounding ISM, which could produce emission consistent with an FRB. The inferred distance for the Lorimer burst in this scenario, however, is calculated to be <20 kpc. This would place the source within our galaxy, and thus the theory is rendered void.		When a BH evaporates to some critical mass, a fireball of electron-positron pairs can be created. The relativistic pairs expand into the magnetic field of the surrounding ISM, which could produce emission consistent with an FRB. The inferred distance for the Lorimer burst in this scenario, however, is calculated to be <20 kpc. This would place the source within our galaxy, and thus the theory is rendered void.

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

	--		--

Jake Gordin: /* Observational Constraints */

2018-10-11T11:24:19Z

Observational Constraints

← Older revision		Revision as of 07:24, 11 October 2018
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	== Observational Constraints ==		== Observational Constraints ==
	~~N/A~~
			--

Jake Gordin at 09:20, 11 October 2018

2018-10-11T09:20:16Z

← Older revision		Revision as of 05:20, 11 October 2018
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	\|GWCounterpart = N/A		\|GWCounterpart = N/A
	\|NeutrinoCounterpart = N/A		\|NeutrinoCounterpart = N/A
	\|References = ~~https~~://~~arxiv~~.~~org~~/~~pdf~~/1206.4135~~.pdf~~		\|References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1206.4135
	\|Comments = None		\|Comments = None
	}}		}}

Emma Platts at 18:06, 10 October 2018

2018-10-10T18:06:59Z

← Older revision		Revision as of 14:06, 10 October 2018
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	\|Progenitor = Annihilating Mini BHs		\|Progenitor = Annihilating Mini BHs
	\|Type = Single		\|Type = Single
	\|EnergyMechanism = -		\|EnergyMechanism = N/A
	\|EmissionMechanism = -		\|EmissionMechanism = N/A
	\|LFRadioCounterpart = -		\|LFRadioCounterpart = N/A
	\|HFRadioCounterpart = -		\|HFRadioCounterpart = N/A
	\|MicrowaveCounterpart = -		\|MicrowaveCounterpart = N/A
	\|THzCounterpart = -		\|THzCounterpart = N/A
	\|OIRCounterpart = -		\|OIRCounterpart = N/A
	\|XrayCounterpart = -		\|XrayCounterpart = N/A
	\|GammarayCounterpart = -		\|GammarayCounterpart = N/A
	\|GWCounterpart = -		\|GWCounterpart = N/A
	\|NeutrinoCounterpart = -		\|NeutrinoCounterpart = N/A
	\|References = https://arxiv.org/pdf/1206.4135.pdf		\|References = https://arxiv.org/pdf/1206.4135.pdf
	\|Comments = None		\|Comments = None
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	== Model Description ==		== Model Description ==

	When a BH evaporates to some critical mass, a fireball of e+~~/e−~~ pairs can be created. The relativistic pairs expand into the magnetic field of the surrounding ISM, which~~, for a sufficiently low mass BH,~~ could produce a emission consistent with an FRB.		When a BH evaporates to some critical mass, a fireball of $e^+_-$ pairs can be created. The relativistic pairs expand into the magnetic field of the surrounding ISM, which could produce emission consistent with an FRB. The inferred distance for the Lorimer burst in this scenario, however, is calculated to be <20 kpc. This would place the source within our galaxy, and thus the theory is rendered void.

	== Observational Constraints ==		== Observational Constraints ==
			N/A
	~~In this scenario the inferred distance to the Lorimer burst is calculated to be <= 20 kpc, putting the source within out Galaxy. This theory is considered inviable.~~

Apw: /* Observational Constraints */

2018-10-09T12:59:22Z

Observational Constraints

← Older revision		Revision as of 08:59, 9 October 2018
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	== Observational Constraints ==		== Observational Constraints ==

	In this scenario the inferred distance to the Lorimer burst is calculated to be ~~200~~ kpc ~~-- far too low~~, ~~thus making this~~ theory inviable.		In this scenario the inferred distance to the Lorimer burst is calculated to be <= 20 kpc, putting the source within out Galaxy. This theory is considered inviable.

Apw: /* Model Description */

2018-10-09T12:16:15Z

Model Description

← Older revision		Revision as of 08:16, 9 October 2018
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	== Model Description ==		== Model Description ==

	When a BH evaporates to some critical mass, a fireball of e+− pairs can be created. The relativistic pairs expand into the magnetic field of the surrounding ISM, which, for a sufficiently low mass BH, could produce a emission consistent with an FRB.		When a BH evaporates to some critical mass, a fireball of e+/e− pairs can be created. The relativistic pairs expand into the magnetic field of the surrounding ISM, which, for a sufficiently low mass BH, could produce a emission consistent with an FRB.

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

	In this scenario the inferred distance to the Lorimer burst is calculated to be 200 kpc -- far too low, thus making this theory inviable.		In this scenario the inferred distance to the Lorimer burst is calculated to be 200 kpc -- far too low, thus making this theory inviable.

Apw: /* Observational Constraints */

2018-10-09T12:14:12Z

Observational Constraints

← Older revision		Revision as of 08:14, 9 October 2018
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	== Observational Constraints ==		== Observational Constraints ==

	In this scenario the inferred distance to the Lorimer burst is calculated to be 200 kpc -- far too ~~little~~, thus making this theory inviable.		In this scenario the inferred distance to the Lorimer burst is calculated to be 200 kpc -- far too low, thus making this theory inviable.

Apw at 12:13, 9 October 2018

2018-10-09T12:13:26Z

← Older revision		Revision as of 08:13, 9 October 2018
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	\|Progenitor = Annihilating Mini BHs		\|Progenitor = Annihilating Mini BHs
	\|Type = Single		\|Type = Single
	\|EnergyMechanism = ~~N/A~~		\|EnergyMechanism = -
	\|EmissionMechanism = ~~N/A~~		\|EmissionMechanism = -
	\|LFRadioCounterpart = ~~N/A~~		\|LFRadioCounterpart = -
	\|HFRadioCounterpart = ~~N/A~~		\|HFRadioCounterpart = -
	\|MicrowaveCounterpart = ~~N/A~~		\|MicrowaveCounterpart = -
	\|THzCounterpart = ~~N/A~~		\|THzCounterpart = -
	\|OIRCounterpart = ~~N/A~~		\|OIRCounterpart = -
	\|XrayCounterpart = ~~N/A~~		\|XrayCounterpart = -
	\|GammarayCounterpart = ~~N/A~~		\|GammarayCounterpart = -
	\|GWCounterpart = ~~N/A~~		\|GWCounterpart = -
	\|NeutrinoCounterpart = ~~N/A~~		\|NeutrinoCounterpart = -
	\|References = https://arxiv.org/pdf/1206.4135.pdf		\|References = https://arxiv.org/pdf/1206.4135.pdf
	\|Comments = None		\|Comments = None

Apw at 12:12, 9 October 2018

2018-10-09T12:12:46Z

← Older revision		Revision as of 08:12, 9 October 2018
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	== Observational Constraints ==		== Observational Constraints ==

	~~N/A~~		In this scenario the inferred distance to the Lorimer burst is calculated to be 200 kpc -- far too little, thus making this theory inviable.

Apw: /* Model Description */

2018-10-09T12:10:53Z

Model Description

← Older revision		Revision as of 08:10, 9 October 2018
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	== Model Description ==		== Model Description ==

	**To fill in with ~~updated draft~~		When a BH evaporates to some critical mass, a fireball of e+− pairs can be created. The relativistic pairs expand into the magnetic field of the surrounding ISM, which, for a sufficiently low mass BH, could produce a emission consistent with an FRB.

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

	N/A		N/A