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arxiv: 1302.6626 · v2 · pith:DZMUESNVnew · submitted 2013-02-26 · 🌌 astro-ph.HE · cond-mat.supr-con· hep-ph· nucl-th

Stellar Superfluids

Dany Page (1) , James M. Lattimer (2) , Madappa Prakash (3) , Andrew W. Steiner (4) ((1) Instituto de Astronomia , Universidad Nacional Autonoma de Mexico , Mexico , (2) Department of Physics , Astronomy
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State University of New York at Stony Brook Stony Brook USA (3) Department of Physics Ohio University Athens (4) Institute for Nuclear Theory University of Washington Seattle USA)
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classification 🌌 astro-ph.HE cond-mat.supr-conhep-phnucl-th
keywords neutronstarspairingnucleinucleonobservedsincesuperfluidity
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Neutron stars provide a fertile environment for exploring superfluidity under extreme conditions. It is not surprising that Cooper pairing occurs in dense matter since nucleon pairing is observed in nuclei as energy differences between even-even and odd-even nuclei. Since superfluids and superconductors in neutron stars profoundly affect neutrino emissivities and specific heats, their presence can be observed in the thermal evolution of neutron stars. An ever-growing number of cooling neutron stars, now amounting to 13 thermal sources, and several additional objects from which upper limits to temperatures can be ascertained, can now be used to discriminate among theoretical scenarios and even to dramatically restrict properties of nucleon pairing at high densities. In addition, observations of pulsars, including their spin-downs and glitch histories, additionally support the conjecture that superfluidity and superconductivity are ubiquitous within, and important to our understanding of, neutron stars.

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Cited by 2 Pith papers

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