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Vortex structure of neutron stars with triplet neutron superfluidity

“…Equations (30) and (31) are the same as those for isotropic 1 S 0 neutron superfluidity [26,27]. Taking 12 2 10 − = ξ cm, 11 10 − = λ…”

“…The interaction between the neutron and proton condensates leads to the entrainment of the superconducting protons by the rotating superfluid neutrons [21,22]. Entrainment around a neutron vortex produces a nonzero proton current which leads to the development of a magnetic flux Φ 1 at the neutron vortex that is not a multiple of Φ 0 [23,24], and to the appearance of an entrainment magnetic field that generates new proton vortices with flux Φ 0 [25]. A nonuniform cluster of proton vortices develops in the region surrounding a neutron vortex, where ( )…”

“…The average magnetic induction of a neutron star owing to these clusters is on the order of 10 12 G [26,27]. The effect of these clusters on the rotational dynamics of pulsars has been examined [28] and the entrainment effect in a solution of 3 He in 4 He has been studied [29].…”

“…The effect of these clusters on the rotational dynamics of pulsars has been examined [28] and the entrainment effect in a solution of 3 He in 4 He has been studied [29]. Neutron superfluids in the 1 S 0 state have discussed in studies of the entrainment effect [21][22][23][24][25][26][27][28].…”

“…Cooper pairs of neutrons and protons are bound states of Fermi quasiparticles, whose properties are essentially unchanged when superfluidity develops. Thus, as in the case of 1 S 0 neutron superfluidity[22,23], the superfluid motion of a3 P 2 condensate of neutron Cooper pairs must be accompanied by proton mass transfer. Here only a part of the superfluid protons are entrained.…”