Axion Cloud and BH: Difference between revisions
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|GWCounterpart = Yes | |GWCounterpart = Yes | ||
|NeutrinoCounterpart = -- | |NeutrinoCounterpart = -- | ||
|References = | |References = http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1709.06581 | ||
|Comments = Observational counterparts could be associated with electron-positron annihilation and/or positronium. | |Comments = Observational counterparts could be associated with electron-positron annihilation and/or positronium. | ||
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== Model Description == | == Model Description == | ||
Spinning BHs have superradiant instabilities, and thus may be surrounded by a dense superradiant axion cloud. Similarly to how a laser can be generated by stimulated axion decay in dense axion clusters, a laser can be triggered in superradiant axion clusters. Such is known as a black hole laser powered by axion superradiant instabilities (BLAST). For a BLAST’s emission to be consistent with FRB observations, the required mass dictates that the BHs be primordial. However, because PBHs form when over densities of gas collapse, they do not have spin, and are unlikely to spin up via accretion. The merging of two PBHs is thus considered for FRBs, where the required spin and resultant superradiant instabilities can be induced. Repeating bursts could occur: the BLAST will form a photon plasma that blocks axion decay and thus halts lasing until e+/e− annihilation reduces the plasma density, and the process can restart. | |||
== Observational Constraints == | == Observational Constraints == | ||
Observational counterparts could be associated with electron-positron annihilation and/or positronium (a bound particle of an electron and positron), though these are not specified. GWs are also expected. | |||
Latest revision as of 03:57, 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 | Superradiant Axion Cloud and BH | Repeat | Laser | Synch. | Yes | -- | -- | -- | -- | -- | -- | Yes | -- | http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1709.06581 | Observational counterparts could be associated with electron-positron annihilation and/or positronium. |
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
Model Description
Spinning BHs have superradiant instabilities, and thus may be surrounded by a dense superradiant axion cloud. Similarly to how a laser can be generated by stimulated axion decay in dense axion clusters, a laser can be triggered in superradiant axion clusters. Such is known as a black hole laser powered by axion superradiant instabilities (BLAST). For a BLAST’s emission to be consistent with FRB observations, the required mass dictates that the BHs be primordial. However, because PBHs form when over densities of gas collapse, they do not have spin, and are unlikely to spin up via accretion. The merging of two PBHs is thus considered for FRBs, where the required spin and resultant superradiant instabilities can be induced. Repeating bursts could occur: the BLAST will form a photon plasma that blocks axion decay and thus halts lasing until e+/e− annihilation reduces the plasma density, and the process can restart.
Observational Constraints
Observational counterparts could be associated with electron-positron annihilation and/or positronium (a bound particle of an electron and positron), though these are not specified. GWs are also expected.