Abstract
This review focuses on applications of the ideas of superfluidity and superconductivity in neutron stars in a broader context, ranging from the microphysics of pairing in nucleonic superfluids to macroscopic manifestations of superfluidity in pulsars. The exposition of the basics of pairing, vorticity and mutual friction can serve as an introduction to the subject. We also review some topics of recent interest, including the various types of pinning of vortices, glitches, and oscillations in neutron stars containing superfluid phases of baryonic matter.
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Notes
- 1.
When computing the variation with respect to the occupation numbers one needs to assume that the Bogolyubov coefficients are constant, because they are determined from the condition δ(E − μN)∕δv p = 0.
- 2.
The full nuclear interaction can be renormalized via resummations of infinite series such as to contain only components close to the Fermi surface.
- 3.
Note that the tensor coupling arises also in the case of pairing in the 3S 1-3D 1 channel which acts only between neutrons and protons and is relevant when the isospin asymmetry between neutrons and protons in not too large (Lombardo et al. 2001).
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Acknowledgements
B.H. has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No. 702713. A.S. is supported by the Deutsche Forschungsgemeinschaft (Grant No. SE 1836/3-2). We acknowledge the support by the NewCompStar COST Action MP1304 and by the PHAROS COST Action CA 16214.
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Haskell, B., Sedrakian, A. (2018). Superfluidity and Superconductivity in Neutron Stars. In: Rezzolla, L., Pizzochero, P., Jones, D., Rea, N., Vidaña, I. (eds) The Physics and Astrophysics of Neutron Stars. Astrophysics and Space Science Library, vol 457. Springer, Cham. https://doi.org/10.1007/978-3-319-97616-7_8
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