Axion Star and BH - Revision history

Emma Platts at 09:03, 12 October 2018

2018-10-12T09:03:52Z

← Older revision		Revision as of 05:03, 12 October 2018
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	\|EnergyMechanism = Electron oscillation		\|EnergyMechanism = Electron oscillation
	\|EmissionMechanism = --		\|EmissionMechanism = --
	\|LFRadioCounterpart = Yes ~~(Circular Polarization)~~		\|LFRadioCounterpart = Yes
	\|HFRadioCounterpart = --		\|HFRadioCounterpart = --
	\|MicrowaveCounterpart = --		\|MicrowaveCounterpart = --
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	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1707.04827		\|References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1707.04827
	\|Comments =		\|Comments = None
	}}		}}

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

	If an axion star ~~were~~ captured by a BH with a strongly magnetized accretion disk, the axion star’s orbit will lead it to approach and impact the accretion disk several times at different locations. The electric field induced by the axion star passing through a strong magnetic field will result in the coherent oscillation of surrounding electrons. The axion star will likely make several impacts before evaporating or eventually being absorbed by the BH.		If an axion star is captured by a BH with a strongly magnetized accretion disk, the axion star’s orbit will lead it to approach and impact the accretion disk several times at different locations. The electric field induced by the axion star passing through a strong magnetic field will result in the coherent oscillation of surrounding electrons. The axion star will likely make several impacts before evaporating or eventually being absorbed by the BH.

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

	The frequency of the radiation will depend on the velocity of the accretion disk at the point of impact. In this way, the variation in central burst frequencies of FRB 121102 can be explained. The intrinsic emission frequency is finite, FRBs would be circularly polarized, and no counterparts are expected.		The frequency of the radiation will depend on the velocity of the accretion disk at the point of impact. In this way, the variation in central burst frequencies of FRB 121102 can be explained. The intrinsic emission frequency is finite, FRBs would be circularly polarized, and no counterparts are expected.

Jake Gordin at 09:30, 11 October 2018

2018-10-11T09:30:10Z

← Older revision		Revision as of 05:30, 11 October 2018
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	\|GWCounterpart = --		\|GWCounterpart = --
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = ~~https~~://~~arxiv~~.~~org~~/~~pdf~~/1707.04827~~.pdf~~		\|References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1707.04827
	\|Comments =		\|Comments =
	}}		}}

Apw: /* Model Description */

2018-10-10T10:27:41Z

Model Description

← Older revision		Revision as of 06:27, 10 October 2018
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	== Model Description ==		== Model Description ==

	If an axion star were captured by a BH with a strongly magnetized accretion disk, the axion star’s orbit will lead it to approach and impact the accretion disk several times at different locations. The electric field induced by the axion star passing through a strong magnetic field will result in the coherent oscillation of surrounding electrons.		If an axion star were captured by a BH with a strongly magnetized accretion disk, the axion star’s orbit will lead it to approach and impact the accretion disk several times at different locations. The electric field induced by the axion star passing through a strong magnetic field will result in the coherent oscillation of surrounding electrons. The axion star will likely make several impacts before evaporating or eventually being absorbed by the BH.

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

	The frequency of the radiation will depend on the velocity of the accretion disk at the point of impact. In this way, the variation in central burst frequencies of FRB 121102 can be explained. The intrinsic emission frequency is finite, FRBs would be circularly polarized, and no counterparts are expected.		The frequency of the radiation will depend on the velocity of the accretion disk at the point of impact. In this way, the variation in central burst frequencies of FRB 121102 can be explained. The intrinsic emission frequency is finite, FRBs would be circularly polarized, and no counterparts are expected.

Apw: /* Observational Constraints */

2018-10-10T10:27:22Z

Observational Constraints

← Older revision		Revision as of 06:27, 10 October 2018
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	== Observational Constraints ==		== Observational Constraints ==

	The frequency of the radiation will depend on the velocity of the accretion disk at the point of impact. In this way, the variation in central burst frequencies of FRB 121102 can be explained. ~~The axion star will likely make several impacts before evaporating or eventually being absorbed by the BH.~~ The intrinsic emission frequency is finite, FRBs would be circularly polarized, and no counterparts are expected.		The frequency of the radiation will depend on the velocity of the accretion disk at the point of impact. In this way, the variation in central burst frequencies of FRB 121102 can be explained. The intrinsic emission frequency is finite, FRBs would be circularly polarized, and no counterparts are expected.

Apw at 10:05, 10 October 2018

2018-10-10T10:05:30Z

← Older revision		Revision as of 06:05, 10 October 2018
Line 9:		Line 9:
	\|EnergyMechanism = Electron oscillation		\|EnergyMechanism = Electron oscillation
	\|EmissionMechanism = --		\|EmissionMechanism = --
	\|LFRadioCounterpart = Yes		\|LFRadioCounterpart = Yes (Circular Polarization)
	\|HFRadioCounterpart = --		\|HFRadioCounterpart = --
	\|MicrowaveCounterpart = --		\|MicrowaveCounterpart = --
Line 19:		Line 19:
	\|NeutrinoCounterpart = --		\|NeutrinoCounterpart = --
	\|References = https://arxiv.org/pdf/1707.04827.pdf		\|References = https://arxiv.org/pdf/1707.04827.pdf
	\|Comments = ~~None~~		\|Comments =
	}}		}}

Apw: /* Observational Constraints */

2018-10-10T09:59:18Z

Observational Constraints

← Older revision		Revision as of 05:59, 10 October 2018
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	== Observational Constraints ==		== Observational Constraints ==

	To be ~~filled in with updated draft~~		The frequency of the radiation will depend on the velocity of the accretion disk at the point of impact. In this way, the variation in central burst frequencies of FRB 121102 can be explained. The axion star will likely make several impacts before evaporating or eventually being absorbed by the BH. The intrinsic emission frequency is finite, FRBs would be circularly polarized, and no counterparts are expected.

Apw: /* Model Description */

2018-10-10T09:59:01Z

Model Description

← Older revision		Revision as of 05:59, 10 October 2018
Line 24:		Line 24:
	== Model Description ==		== Model Description ==

	~~To be filled~~ in ~~with updated draft~~		If an axion star were captured by a BH with a strongly magnetized accretion disk, the axion star’s orbit will lead it to approach and impact the accretion disk several times at different locations. The electric field induced by the axion star passing through a strong magnetic field will result in the coherent oscillation of surrounding electrons.

	== 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 = Collision..."

2018-10-02T12:51:25Z

Created page with "   {{FRBTableTemplate |Category = Collision..."

New page

{{FRBTableTemplate
|Category = Collision / Interaction
|Progenitor = Axion Star and BH
|Type = Repeat
|EnergyMechanism = Electron oscillation
|EmissionMechanism = --
|LFRadioCounterpart = Yes
|HFRadioCounterpart = --
|MicrowaveCounterpart = --
|THzCounterpart = --
|OIRCounterpart = --
|XrayCounterpart = --
|GammarayCounterpart = --
|GWCounterpart = --
|NeutrinoCounterpart = --
|References = https://arxiv.org/pdf/1707.04827.pdf
|Comments = None
}}

== Model Description ==

To be filled in with updated draft

== Observational Constraints ==

To be filled in with updated draft