Superfluidity in Disordered Neutron Stars Crusts

J. A. Sauls; N. Chamel; M. A. Alpar

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arXiv · 2001.09959

Superfluidity in Disordered Neutron Stars Crusts

J. A. Sauls·N. Chamel·M. A. Alpar

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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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astro-ph.HE cond-mat.supr-con nucl-th

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J. A. Sauls, N. Chamel, M. A. Alpar. 2020-01-27. Superfluidity in Disordered Neutron Stars Crusts. https://arxiv.org/abs/2001.09959

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