Pith. sign in

REVIEW 3 cited by

Stellar Superfluids

Not yet reviewed by Pith; the record is open.

Re-run · record.json Download PDF Read on arXiv ↗

This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.

SPECIMEN: schema-true, not a live event

T0 review · schema-true

One-sentence machine reading of the paper's core claim.

pith:XXXXXXXX · record.json · timestamp

arxiv 1302.6626 v2 pith:DZMUESNV submitted 2013-02-26 astro-ph.HE cond-mat.supr-conhep-phnucl-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
show 10 more authors
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)
This is my paper
classification astro-ph.HE cond-mat.supr-conhep-phnucl-th
keywords neutronstarspairingnucleinucleonobservedsincesuperfluidity
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved
0 comments
read the original abstract

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.

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Forward citations

Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Cooling of Hybrid Stars with a 2SC+$<dd>$ Phase

    nucl-th 2026-06 unverdicted novelty 7.0

    Hybrid stars containing the 2SC+<dd> phase cool more slowly than those with the 2SC phase because inherited 3P2 superfluidity suppresses quark beta decay, producing cooling curves close to the CFL case.

  2. Neutron star heating vs. HST observations

    astro-ph.HE 2025-11 unverdicted novelty 5.0

    A combination of rotochemical heating with a large pairing gap and vortex creep explains the observed temperatures of PSR J0437-4715 and PSR B0950+08 while remaining consistent with upper limits on three other old pulsars.

  3. Cooling of Isolated Neutron Stars with Hyperon-mixed Kaon-Condensation Matter

    astro-ph.HE 2026-05 unverdicted novelty 4.0

    Strong proton superconductivity at high densities shuts down nucleon and hyperon direct Urca cooling, making kaon-induced Urca processes dominant and explaining cold massive neutron stars.