Nature of fault planes in solid neutron star matter

@article{Jones2002NatureOF,
  title={Nature of fault planes in solid neutron star matter},
  author={P. B. Jones},
  journal={arXiv: Astrophysics},
  year={2002}
}
The properties of tectonic earthquake sources are compared with those deduced here for fault planes in solid neutron-star matter. The conclusion that neutron-star matter cannot exhibit brittle fracture at any temperature or magnetic field is significant for current theories of pulsar glitches, and of the anomalous X-ray pulsars and soft-gamma repeaters. 
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References

SHOWING 1-10 OF 24 REFERENCES
Liquid Crystals in the Mantles of Neutron Stars
Recent calculations indicate that in the outer parts of neutron stars nuclei are rod-like or slab-like, rather than roughly spherical. We consider the elastic properties of these phases, and argueExpand
Earthquake-like behaviour of soft γ-ray repeaters
NEUTRON stars are believed to have solid crusts, which may exhibit tectonic activity analogous to earthquakes on Earth. These 'starquakes' have been invoked to explain several phenomena associatedExpand
Progressive Deformation of the Crust of Pulsars
It is shown that the crust of pulsars can deform in a gradual plastic manner in spite of its extreme density and strength. This deformation leads to stronger damping of pulsar rotation and to higherExpand
First-principles point-defect calculations for solid neutron star matter
Formation enthalpies are calculated for a number of point-defect structures in solid neutron star matter at densities above the neutron-drip threshold. The enthalpies obtained show that an amorphousExpand
The Mechanics of Earthquakes and Faulting
Preface Acknowledgments List of symbols 1. Brittle fracture of rock 2. Rock friction 3. Mechanics of faulting 4. Mechanics of earthquakes 5. The seismic cycle 6. Seismotectonics 7. EarthquakeExpand
Neutron Star Magnetic Field Evolution, Crust Movement, and Glitches: Erratum
Spinning superfluid neutrons in the core of a neutron star interact strongly with coexisting superconducting protons. One consequence is that the outward (inward) motion of core superfluid neutronExpand
Powering Anomalous X-Ray Pulsars by Neutron Star Cooling
Using recently calculated analytic models for the thermal structure of ultramagnetized neutron stars, we estimate the thermal fluxes from young (t~1000 yr) ultramagnetized (B~1015 G) cooling neutronExpand
Starquake-induced Magnetic Field and Torque Evolution in Neutron Stars
The persistent increases in spin-down rate (offsets) seen to accompany glitches in the Crab and other pulsars suggest increases in the spin-down torque. We interpret these offsets as due toExpand
The Soft Gamma Repeaters as Very Strongly Magnetized Neutron Stars. II. Quiescent Neutrino, X-Ray, and Alfvén Wave Emission
We calculate the quiescent X-ray, neutrino, and Alfven wave emission from a neutron star with a very strong magnetic field, Bdipole ~ 1014 − 1015 G and Binterior ~ (5–10) × 1015 G. These results areExpand
Neutron starquake models for gamma-ray bursts
We assess neutron starquake models for γ-ray bursts. The elastic energy the crust can store is sufficient to account for that radiated in a single burst, but it is insufficient to supply the ≳ 10^6Expand
...
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