Difference between revisions of "Starquakes"

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|XrayCounterpart        = Yes
 
|XrayCounterpart        = Yes
 
|GammarayCounterpart    = Yes <br/> if jet aligned
 
|GammarayCounterpart    = Yes <br/> if 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 of a pulsar have been considered as a source of repeating FRBs. The bursts of FRB 121102 are consistent with the aftershock sequence of an earthquake, where the burst’s time-decaying rate of seismicity falls within the typical values of earthquakes. They also show that the burst energy distribution of FRB 121102 has a power law form, much like that of the Gutenberg-Richter law of earthquakes. Further, the waiting time of bursts has a Gaussian distribution; another characteristic feature of earthquakes.  
+
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 are poorly understood, limiting the testability of this theory. They may be associated with SGRs, which offers counterparts for which to search.
+
Starquakes may be associated with SGRs or magentar flares, which offers counterparts for which to search.

Revision as of 07:07, 6 September 2019





Summary Table
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 -- -- -- -- Yes Yes
if 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.