AGN-SS: Difference between revisions
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Latest revision as of 03:55, 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 | |||||||
| AGN | AGN-Strange Star Interaction | Repeat | Electron oscillation | -- | Yes | -- | -- | -- | Thermal | -- | Yes | Yes | Yes | http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1709.00185 | Neutrinos from preceding SN and from collapse to BH. GW from collapse and persistent GWs from SS. |
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
Model Description
A strange quark star (SS) is made up of approximately the same number of up, down, and strange quarks, with a small number of electrons distributed across the star's surface. Should an AGN wind interact with a SS, it can induce torsional oscillation of the electron layer relative to the positively charged SS, which can emit high luminosity GHz radio waves, consistent with FRBs. The sporadic nature of AGN wind would induce a repeating FRB.
Observational Constraints
Persistent gravitational waves are expected from the SS due to its r-mode instability. If the SS is the result of a spinning down magnetar, neutrinos and a GW could be released when the magnetar collapses, however this emission need not be close in time to the interaction of the SS with the AGN, making it difficult to draw any associations.