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Superfluid Density of Neutrons in the Inner Crust of Neutron Stars: New Life for Pulsar Glitch Models
Zhejiang Univ, Dept Phys, Hangzhou 310027, Zhejiang, Peoples R China.;Zhejiang Univ, Zhejiang Inst Modern Phys, Hangzhou 310027, Zhejiang, Peoples R China..
KTH, Centra, Nordic Institute for Theoretical Physics NORDITA. Univ Copenhagen, Niels Bohr Int Acad, Niels Bohr Inst, Blegdamsvej 17, DK-2100 Copenhagen O, Denmark.
2017 (engelsk)Inngår i: Physical Review Letters, ISSN 0031-9007, E-ISSN 1079-7114, Vol. 119, nr 6, artikkel-id 062701Artikkel i tidsskrift (Fagfellevurdert) Published
Abstract [en]

Calculations of the effects of band structure on the neutron superfluid density in the crust of neutron stars made under the assumption that the effects of pairing are small [N. Chamel, Phys. Rev. C 85, 035801 (2012)] lead to moments of inertia of superfluid neutrons so small that the crust alone is insufficient to account for the magnitude of neutron star glitches. Inspired by earlier work on ultracold atomic gases in an optical lattice, we investigate fermions with attractive interactions in a periodic lattice in the mean-field approximation. The effects of band structure are suppressed when the pairing gap is of order or greater than the strength of the lattice potential. By applying the results to the inner crust of neutron stars, we conclude that the reduction of the neutron superfluid density is considerably less than previously estimated and, consequently, it is premature to rule out models of glitches based on neutron superfluidity in the crust.

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American Physical Society, 2017. Vol. 119, nr 6, artikkel-id 062701
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URN: urn:nbn:se:kth:diva-243517DOI: 10.1103/PhysRevLett.119.062701ISI: 000407326800005PubMedID: 28949649Scopus ID: 2-s2.0-85027845549OAI: oai:DiVA.org:kth-243517DiVA, id: diva2:1287359
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QC 20190211

Tilgjengelig fra: 2019-02-11 Laget: 2019-02-11 Sist oppdatert: 2019-02-11bibliografisk kontrollert

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