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- W1883231489 abstract "As the number of nucleons in stable atomic nuclei increases, their neutron to proton ratios grow larger. So does the fraction of each atom's electrons which is contained within its nuclear volume. If an atomic weight (A) were to exceed 104 that atom would resemble a canonical neutron star: a huge nucleus consisting mainly of neutrons, several percent protons, and an electron cloud almost entirely contained within the nucleus. In the commonly observed nuclei this limit cannot be reached because nucleon-nucleon attractive forces can no longer prevent nuclear fission from Coulomb repulsion when A exceeds 300. However, if A were to reach 1055, gravitational attraction would become sufficiently strong to hold the star together and we can have a stable conventional neutron star. In it, the dominant neutron sea is a quantum fluid with properties very similar to those of very low temperature superfluid Helium. The much less abundant protons form a superconductor whose properties closely resemble those of a BCS (Bardeen, Cooper, Schrieffer) electron superconductor. Both of these quantum fluids are well understood and their expected properties confirmed in laboratory experiments. Most astrophysically relevant features do not depend on the fermion masses or fluid densities and lead to the model presented below for various phenomena in the development of a canonical neutron star. In a cooled core below the relatively thin crust of a spinning neutron star (NS) superconducting protons (SC-p)coexist with much more abundant superfluid neutrons (SF-n) to form a giant atomic nucleus which contains within it a neutralizing sea of degenerate ultra-relativistic electrons. Superfluid neutrons in a star with a spin-period P(sec) rotate by forming a nearly uniform array of co-rotating quantized vortex lines parallel to the star's spin axis. This array has a number of vortices per unit area density nv ~ 104 P−1 cm−2 (cf. Fig. 14.1)." @default.
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- W1883231489 date "2009-02-09" @default.
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- W1883231489 title "Pulsar Spin, Magnetic Fields, and Glitches" @default.
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- W1883231489 doi "https://doi.org/10.1007/978-3-540-76965-1_14" @default.
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