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arXiv:astro-ph/0402514 (astro-ph)
[Submitted on 22 Feb 2004 (v1), last revised 10 Sep 2004 (this version, v2)]

Title:Phase Transitions in Nucleonic Matter and Neutron-Star Cooling

Authors:V. A. Khodel, J. W. Clark, M. Takano, M. V. Zverev
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Abstract: A new scenario for neutron-star cooling is proposed, based on the correspondence between pion condensation, occurring in neutron matter due to critical spin-isospin fluctuations, and the metal-insulator phase transition in a two-dimensional electron gas. Beyond the threshold density for pion condensation, where neutron-star matter loses its spatial homogeneity, the neutron single-particle spectrum acquires an insulating gap that quenches neutron contributions to neutrino-production reactions and to the star's specific heat. In the liquid phase at densities below the transition point, spin-isospin fluctuations are found to play dual roles. On the one hand, they lead to a multi-sheeted neutron Fermi surface that extends to low momenta, thereby activating the normally forbidden direct-Urca cooling mechanism; on the other, they amplify the nodeless $P$-wave neutron superfluid gap while suppressing $S$-wave pairing. In this picture, lighter stars without a pion-condensed core experience slow cooling, while enhanced cooling occurs in heavier stars through direct-Urca emission from a narrow shell of the interior.
Comments: 4 pages, 2 figures. Revised version. Accepted for publication in this http URL
Subjects: Astrophysics (astro-ph)
Cite as: arXiv:astro-ph/0402514
  (or arXiv:astro-ph/0402514v2 for this version)
  https://doi.org/10.48550/arXiv.astro-ph/0402514
Journal reference: Phys.Rev.Lett.93:151101,2004
Related DOI: https://doi.org/10.1103/PhysRevLett.93.151101

Submission history

From: Mikhail Zverev [view email]
[v1] Sun, 22 Feb 2004 14:27:37 UTC (69 KB)
[v2] Fri, 10 Sep 2004 12:12:52 UTC (69 KB)
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