Superfluidity in Neutron Star Matter

By U. Lombardo, Hans-Josef Schulze. 2000

138 citations recorded by the source corpus.

The research on the superfluidity of neutron matter can be traced back to Migdal’s observation that neutron stars are good candidates for being macroscopic superfluid systems [1]. And, in fact, during more than two decades of neutron-star physics the presence of neutron and proton superfluid phases has been invoked to explain the dynamical and thermal evolution of a neutron star. The most striking evidence is given by post-glitch timing observations [2],[3], but also the cooling history is strongly influenced by the possible presence of super- fluid phases [4],[5]. On the theoretical side, the onset of superfluidity in neutron matter or in the more general context of nuclear matter was investigated soon after the formulation of the Bardeen, Cooper, and Schrieffer (BCS) theory of superconductivity [6] and the pairing theory in atomic nuclei [7],[8].

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/55e00f2e90d1c439c67e1d058efd10fa046a0f18

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Citations in the corpus

The BCS–BEC crossover: From ultra-cold Fermi gases to nuclear systems (2018, methodology): “[448] (see also references therein) is remedied by dressing the vertex insertions according to the Babu-Brown induced-interaction theory [449].”
Stellar structure models in modified theories of gravity: Lessons and challenges (2019, background): “Moreover, neutron stars are expected to exhibit different phases of superfluidity/superconductivity [17].”
Neutron Stars 1 : Equation of State and Structure (2007, methodology): “Critical temperaturesTc of various particle species have been calculated by many authors as reviewed by Lombardo & Schulze (2001) (more references can be found in Yakovlevet al. 1999).”
Superfluidity in nuclear systems and neutron stars (2018, background): “At the large isospin asymmetries found in neutron stars, where the neutron number density is about 95% of the total baryonic density,2 only T = 1 Cooper pairs can form (Dean and Hjorth-Jensen, 2003; Lombardo and Schulze, 2001).”
Long Type I X-Ray Bursts and Neutron Star Interior Physics (2005, background): “In a medium, many-body effects alter the interaction and much effort has been dedicated to studying them (see, e.g., Lombardo & Schulze 2001 for a review).”
The Nuclear Symmetry Energy (2016, background): “Unfortunately the theoretical estimates of the nuclear pairing gaps in nuclear matter is quite uncertain [102, 103].”