Difference between revisions of "Axion Star and BH"

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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              =  
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|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.

Latest revision as of 05:03, 12 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
Collision / Interaction Axion Star and BH Repeat Electron oscillation -- Yes -- -- -- -- -- -- -- -- http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1707.04827 None

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


Model Description

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

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.