2020/01/27 by J. A. Sauls, N. Chamel, Sauls, J. A. +3 · 14 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics #Condensed matter physics #Crust #FOS: Physical sciences #Geophysics #High Energy Astrophysical Phenomena (astro-ph.HE) #High-pressure geophysics and materials #Neutron #Neutron scattering #Neutron star #Nuclear Physics and Applications #Nuclear Theory (nucl-th) #Nuclear physics #Physics #Pulsar #Pulsars and Gravitational Waves Research #Superconductivity (cond-mat.supr-con) #Superfluidity #astro-ph.HE #cond-mat.supr-con #nucl-th
paper · pdf · doi:10.48550/arxiv.2001.09959
published in arXiv (Cornell University) (Cornell University) · 6 pages, 5 figures
arxiv created 2020/01/27 · openalex publication_date 2020/01/27 · arxiv updated 2020/01/28 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
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, ρs/ρ, at densities above that of neutron drip, ρd ≈ 4× 1011 g/cm3. For an amorphous solid crust the suppression of ρs 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.