Breaking properties of neutron star crust

Baiko, D. A.; Chugunov, A. I.

doi:10.1093/mnras/sty2259

Cited by 99 publications

(100 citation statements)

References 32 publications

(56 reference statements)

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“…This could support significant "mountains" with large asymmetries and ellipticity ǫ as large as 10 −6 to 10 −5 [403]. More recently, Baiko and Chugunov [404] argued that the maximum strain for the stretch deformation sustainable elastically is 0.04. As already mentioned earlier in this review, the physics of the neutron-star crust is a very active area of research and the exact value of σ max is still to be determined.…”

Section: Symmetry Energy Effects On the Ellipticity And Gw Emissions mentioning

confidence: 95%

Towards understanding astrophysical effects of nuclear symmetry energy

et al. 2019

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Determining the Equation of State (EOS) of dense neutron-rich nuclear matter is a shared goal of both nuclear physics and astrophysics. Except possible phase transitions, the density dependence of nuclear symmetry Esym(ρ) is the most uncertain part of the EOS of neutron-rich nucleonic matter especially at supra-saturation densities. Much progresses have been made in recent years in predicting the symmetry energy and understanding why it is still very uncertain using various microscopic nuclear many-body theories and phenomenological models. Simultaneously, significant progresses have also been made in probing the symmetry energy in both terrestrial nuclear laboratories and astrophysical observatories. In light of the GW170817 event as well as ongoing or planned nuclear experiments and astrophysical observations probing the EOS of dense neutron-rich matter, we review recent progresses and identify new challenges to the best knowledge we have on several selected topics critical for understanding astrophysical effects of the nuclear symmetry energy.PACS. 2 6.60.Kp Contents B.A Li, P.G. Krastev, D.H. Wen and N.B. Zhang: Astrophysical Effects of Nuclear Symmetry Energy 5.2.2 Predicted correlation strength between the radii of neutron stars and the symmetry energy from low to high densities 32 5.2.3 Predicted effects of the symmetry energy on the tidal deformability of neutron stars 33 5.3 Post-GW170817 analyses of tidal deformability and radii of neutron stars as well as constraints on the nuclear EOS and symmetry energy . . . 34 5.3.

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Section: Symmetry Energy Effects On the Ellipticity And Gw Emissions mentioning

confidence: 95%

Towards understanding astrophysical effects of nuclear symmetry energy

et al. 2019

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“…where σ is the elastic strain tensor and σmax is the maximum breaking strain of the crust. Baiko & Chugunov 2018). Although depending on various factors, such as the degree of hydrostatic pressure anisotropies, moleculardynamics simulations performed in the aforementioned studies find 10 −3 σmax 10 −1 .…”

Section: Fracturing Crustsmentioning

confidence: 96%

Young magnetars with fracturing crusts as fast radio burst repeaters

Suvorov

Kokkotas

2019

Monthly Notices of the Royal Astronomical Society

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Fast radio bursts are millisecond-duration radio pulses of extragalactic origin. A recent statistical analysis has found that the burst energetics of the repeating source FRB 121102 follow a power-law, with an exponent that is curiously consistent with the Gutenberg-Richter law for earthquakes. This hints that repeat-bursters may be compact objects undergoing violent tectonic activity. For young magnetars, possessing crustal magnetic fields which are both strong (B 10 15 G) and highly multipolar, Hall drift can instigate significant field rearrangements even on century long timescales. This reconfiguration generates zones of magnetic stress throughout the outer layers of the star, potentially strong enough to facilitate frequent crustal failures. In this paper, assuming a quake scenario, we show how the crustal field evolution, which determines the resulting fracture geometries, can be tied to burst properties. Highly anisotropic stresses are generated by the rapid evolution of multipolar fields, implying that small, localised cracks can occur sporadically throughout the crust during the Hall evolution. Each of these shallow fractures may release bursts of energy, consistent in magnitude with those seen in the repeating sources FRB 121102 and FRB 180814.J0422+73.

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“…As remarked earlier, there may even be a time evolution of the magneticfield-induced quadrupole ellipticity in these early phases. This is a plausible scenario assuming that the concerned crustal stresses and strains, due to the magnetic pressure, are below the breaking limit [60,61]. An evolving quadrupole ellipticity has been previously studied, in other GW contexts [62][63][64][65], and we would like to explore if the presence of MMMs may leave imprints on this quadrupole ellipticity evolution, and consequent GW generation.…”

Section: Magnetic Field Induced Quadrupole Momentsmentioning

confidence: 97%

“…This causes a decay of the magnetic field hitherto different from conventional mechanisms operational in a neutron star. The modified magnetic field evolution in turn may affect the time evolution of the quadrupole ellipticity, assuming the concerned neutron star crustal strains are below the breaking limit [60,61]. This opens up an avenue for probing these exotic states by their imprints on the gravitational waves emitted.…”

Section: Introductionmentioning

confidence: 99%

Continuous gravitational waves and magnetic monopole signatures from single neutron stars

2020

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Future observations of continuous gravitational waves from single neutron stars, apart from their monumental astrophysical significance, could also shed light on fundamental physics and exotic particle states. One such avenue is based on the fact that magnetic fields cause deformations of a neutron star, which results in a magnetic-field-induced quadrupole ellipticity. If the magnetic and rotation axes are different, this quadrupole ellipticity may generate continuous gravitational waves which may last decades, and may be observable in current or future detectors. Light, milli-magnetic monopoles, if they exist, could be pair-produced non-perturbatively in the extreme magnetic fields of neutron stars, such as magnetars. This non-perturbative production furnishes a new, direct dissipative mechanism for the neutron star magnetic fields. Through their consequent effect on the magnetic-fieldinduced quadrupole ellipticity, they may then potentially leave imprints in the early stage continuous gravitational wave emissions. We speculate on this possibility in the present study, by considering some of the relevant physics and taking a very simplified toy model of a magnetar as the prototypical system. Preliminary indications are that new-born millisecond magnetars could be promising candidates to look for such imprints. Deviations from conventional evolution, and comparatively abrupt features in the early stage gravitational waveforms, distinct from other astrophysical contributions, could be distinguishable signatures for these exotic monopole states.

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Breaking properties of neutron star crust

Cited by 99 publications

References 32 publications

Towards understanding astrophysical effects of nuclear symmetry energy

Towards understanding astrophysical effects of nuclear symmetry energy

Young magnetars with fracturing crusts as fast radio burst repeaters

Continuous gravitational waves and magnetic monopole signatures from single neutron stars

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