Axion Star and BH: Difference between revisions
Jake Gordin (talk | contribs) No edit summary |
Emma Platts (talk | contribs) No edit summary |
||
| Line 9: | Line 9: | ||
|EnergyMechanism = Electron oscillation | |EnergyMechanism = Electron oscillation | ||
|EmissionMechanism = -- | |EmissionMechanism = -- | ||
|LFRadioCounterpart = Yes | |LFRadioCounterpart = Yes | ||
|HFRadioCounterpart = -- | |HFRadioCounterpart = -- | ||
|MicrowaveCounterpart = -- | |MicrowaveCounterpart = -- | ||
| Line 19: | Line 19: | ||
|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 | 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 04:03, 12 October 2018
| 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.