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Universe 2017, 3(1), 5; doi:10.3390/universe3010005

Quark Deconfinement in Rotating Neutron Stars

1
Department of Physics, San Diego State University, San Diego, CA 92182, USA
2
Department of Physics, University of California, La Jolla, San Diego, CA 92093, USA
3
National Scientific and Technical Research Council (CONICET), Godoy Cruz 2290, Buenos Aires 1425, Argentina
4
Grupo de Gravitación, Astrofísica y Cosmología, Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, La Plata 1900, Argentina
5
Instituto de Física La Plata, National Scientific and Technical Research Council (CONICET), Universidad Nacional de La Plata, La Plata 1900, Argentina
*
Author to whom correspondence should be addressed.
Academic Editors: Roman Pasechnik, José Eliel Camargo-Molina and António Pestana Morais
Received: 29 October 2016 / Revised: 11 January 2017 / Accepted: 15 January 2017 / Published: 24 January 2017
View Full-Text   |   Download PDF [1008 KB, uploaded 24 January 2017]   |  

Abstract

In this paper, we use a three flavor non-local Nambu–Jona-Lasinio (NJL) model, an improved effective model of Quantum Chromodynamics (QCD) at low energies, to investigate the existence of deconfined quarks in the cores of neutron stars. Particular emphasis is put on the possible existence of quark matter in the cores of rotating neutron stars (pulsars). In contrast to non-rotating neutron stars, whose particle compositions do not change with time (are frozen in), the type and structure of the matter in the cores of rotating neutron stars depends on the spin frequencies of these stars, which opens up a possible new window on the nature of matter deep in the cores of neutron stars. Our study shows that, depending on mass and rotational frequency, up to around 8% of the mass of a massive neutron star may be in the mixed quark-hadron phase, if the phase transition is treated as a Gibbs transition. We also find that the gravitational mass at which quark deconfinement occurs in rotating neutron stars varies quadratically with spin frequency, which can be fitted by a simple formula. View Full-Text
Keywords: rotation; quarks; deconfinement; neutron star; pulsar; nuclear equation of state rotation; quarks; deconfinement; neutron star; pulsar; nuclear equation of state
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This is an open access article distributed under the Creative Commons Attribution License which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. (CC BY 4.0).

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MDPI and ACS Style

Mellinger, R.D.; Weber, F.; Spinella, W.; Contrera, G.A.; Orsaria, M.G. Quark Deconfinement in Rotating Neutron Stars. Universe 2017, 3, 5.

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