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DOE OSTI · 1659469

Superfluidity in Disordered Neutron Stars Crusts

Sauls, J. A.·Chamel, N.·Alpar, M. A.
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Abstract

Nonequilibrium conditions imposed by neutrino cooling through the liquid-solid transition lead to disorder in the solid crust of neutron stars. Disorder reduces the superfluid fraction, $\rho_s/\rho$, at densities above that of neutron drip, $\rho_d \approx 4\times 10^{11}\,g/cm^3$. For an amorphous solid crust the suppression of $\rho_s$ is small, except in the highest density regions of the crust. In contrast to the strong reduction in neutron conduction predicted for coherent Bragg scattering in a crystalline crust, the disordered solid crust supports sufficient neutron superfluid density to account for pulsar glitches.

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73 NUCLEAR PHYSICS AND RADIATION PHYSICS79 ASTRONOMY AND ASTROPHYSICS

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BibTeXRIS

Sauls, J. A., Chamel, N., Alpar, M. A.. 2020-01-27. Superfluidity in Disordered Neutron Stars Crusts. https://www.osti.gov/biblio/1659469

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