Heterogeneity of solid neutron‐star matter: transport coefficients and neutrino emissivity

@article{Jones2004HeterogeneityOS,
  title={Heterogeneity of solid neutron‐star matter: transport coefficients and neutrino emissivity},
  author={P. B. Jones},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2004},
  volume={351},
  pages={956-966}
}
  • P. B. Jones
  • Published 17 March 2004
  • Physics
  • Monthly Notices of the Royal Astronomical Society
Calculations of weak-interaction transition rates and of nuclear formation enthalpies show that in isolated neutron stars, the solid phase, above the neutron-drip threshold, is amorphous and heterogeneous in nuclear charge. The neutrino emissivities obtained are very dependent on the effects of proton shell structure but may be several orders of magnitude larger than the electron bremsstrahlung neutrino pair emissivity at temperatures ∼10 9 K. In this phase, electrical and thermal… 

Figures and Tables from this paper

Type II superconductivity and magnetic flux transport in neutron stars

The transition to a type II proton superconductor which is believed to occur in a cooling neutron star is accompanied by changes in the equation of hydrostatic equilibrium and by the formation of

Many-body Problems in the Theory of Stellar Collapse and Neutron Stars

When modelling the collapse of massive stars leading to supernova explosions and the cooling of neutron stars, understanding the microphysical processes, such as the interaction of neutrinos within a

Atmospheres and radiating surfaces of neutron stars

The early 21st century is witnessing a breakthrough in the study of the thermal radiation of neutron stars. Observations with modern space telescopes have provided a wealth of valuable information,

Anisotropic thermal emission from magnetized neutron stars

Context. The thermal emission from isolated neutron stars is not well understood. The X-ray spectrum is very close to a blackbody but there is a systematic optical excess flux with respect to the

Neutron star cooling after deep crustal heating in the X-ray transient KS 1731–260

We simulate the cooling of the neutron star in the X-ray transient KS 1731−260 after the source returned to quiescence in 2001 from a long (≳12.5 yr) outburst state. We show that the cooling can be

Superburst Ignition and Implications for Neutron Star Interiors

Superbursts are thought to be powered by the unstable ignition of a carbon-enriched layer formed from the burning of accreted hydrogen and helium. As shown by Cumming & Bildsten, the short recurrence

Constraints on the symmetry energy from observational probes of the neutron star crust

A number of observed phenomena associated with individual neutron star systems or neutron star populations find explanations in models in which the neutron star crust plays an important role. We

The bottom magnetic field and magnetosphere evolution of neutron star in low-mass X-ray binary

The accretion-induced neutron star (NS) magnetic field evolution is studied through considering the accretion flow to drag the field lines aside and dilute the polar-field strength, and as a result

Long Type I X-Ray Bursts and Neutron Star Interior Physics

Two types of long-duration type I X-ray bursts have been discovered by long-term monitoring observations of accreting neutron stars: superbursts and ``intermediate duration'' bursts. We investigate

References

SHOWING 1-10 OF 42 REFERENCES

Thermal structure and cooling of neutron stars with magnetized envelopes

The thermal structure of neutron stars with magnetized envelopes is studied using modern physics input. The relation between the internal (Tint) and local surface temperatures is calculated and tted

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 amorphous

Neutron star crusts.

TLDR
Property of neutron star matter at subnuclear densities using an improved nuclear Hamiltonian is calculated, finding that the thinner crust and the unusual nuclear shape have important consequences for theories of the rotational and thermal evolution of neutron stars, especialy theories of glitches.

Electron screening in the liquid-gas mixed phases of nuclear matter

Screening effects of electrons on inhomogeneous nuclear matter, which includes spherical, slablike, and rodlike nuclei as well as spherical and rodlike nuclear bubbles, are investigated in view of

Crustal magnetic field decay and neutron star cooling

The ohmic decay of the magnetic field initially confined to the surface layers of the neutron star crust is considered. It is shown that the neutron star cooling can effectively increase the

Neutron star matter at sub-nuclear densities

Non-linear magnetic field decay in neutron stars Theory and observations

There exists both theoretical and observational evidence that the magnetic field decay in neutron stars may proceed in a pronounced non-linear way during a certain episode of the neutron star's life.