Axion Minicluster and NS: Difference between revisions
Jump to navigation
Jump to search
| Line 28: | Line 28: | ||
== Observational Constraints == | == Observational Constraints == | ||
The predicted emission timescale, the energetics, luminosities, and event rate are in-keeping with FRB observations. | |||
Revision as of 04:41, 10 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 Minicluster and NS | Single | Maser | Synch. | Yes | -- | -- | -- | -- | -- | -- | -- | -- | http://adsabs.harvard.edu/abs/2015JETPL.101....1T | None |
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
Model Description
Axion clumps with masses below the stellar range, known as Axion Bose Clusters or “miniclusters”, have been considered as FRB progenitors. In the strong magnetic field of a compact object, an instability may arise in a minicluster, causing it to explosively decay into photons via a synchrotron maser mechanism.
Observational Constraints
The predicted emission timescale, the energetics, luminosities, and event rate are in-keeping with FRB observations.