Starquakes: Difference between revisions
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|MicrowaveCounterpart = -- | |MicrowaveCounterpart = -- | ||
|THzCounterpart = -- | |THzCounterpart = -- | ||
|OIRCounterpart = | |OIRCounterpart = Possible | ||
|XrayCounterpart = | |XrayCounterpart = Possible | ||
|GammarayCounterpart = Yes <br/> if jet aligned | |GammarayCounterpart = Yes <br/> if pulsar jet aligned | ||
|GWCounterpart = | |GWCounterpart = Yes, but unlikely detectable | ||
|NeutrinoCounterpart = -- | |NeutrinoCounterpart = -- | ||
|References = http://adsabs.harvard.edu/abs/2018ApJ...852..140W | |References = http://adsabs.harvard.edu/abs/2018ApJ...852..140W, https://arxiv.org/pdf/1907.10394.pdf | ||
|Comments = None | |Comments = None | ||
}} | }} | ||
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== Model Description == | == Model Description == | ||
The starquakes | The starquakes have been considered as a source of repeating FRBs. The aftershock sequence of an earthquake, where the burst’s time-decaying rate of seismicity falls within the typical values of earthquakes. The burst energy distribution of FRB 121102 has a power law form, much like that of the Gutenberg-Richter law of earthquakes. The waiting time of bursts has a Gaussian distribution; another characteristic feature of earthquakes. Young magnetars with strong and highly multipolar crustal magnetic fields can experience significant field rearrangements timescales of <~100 years. Magnetic stresses then occur throughout the outer layers of the star, potentially causing frequent crustal failures. The bursts of FRB 121102 and FRB 180814.J0422+73 are consistent with this picture. | ||
== Observational Constraints == | == Observational Constraints == | ||
Starquakes | Starquakes may be associated with SGRs or magentar flares, which offers counterparts for which to search. | ||
Latest revision as of 07:10, 6 September 2019
| 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 | |||||||
| Other | Starquakes | Repeat | Mag. reconnection | Curv. | Yes | -- | -- | -- | Possible | Possible | Yes if pulsar jet aligned |
Yes, but unlikely detectable | -- | http://adsabs.harvard.edu/abs/2018ApJ...852..140W, https://arxiv.org/pdf/1907.10394.pdf | None |
Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)
Model Description
The starquakes have been considered as a source of repeating FRBs. The aftershock sequence of an earthquake, where the burst’s time-decaying rate of seismicity falls within the typical values of earthquakes. The burst energy distribution of FRB 121102 has a power law form, much like that of the Gutenberg-Richter law of earthquakes. The waiting time of bursts has a Gaussian distribution; another characteristic feature of earthquakes. Young magnetars with strong and highly multipolar crustal magnetic fields can experience significant field rearrangements timescales of <~100 years. Magnetic stresses then occur throughout the outer layers of the star, potentially causing frequent crustal failures. The bursts of FRB 121102 and FRB 180814.J0422+73 are consistent with this picture.
Observational Constraints
Starquakes may be associated with SGRs or magentar flares, which offers counterparts for which to search.