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Deconfinement phase transition in proto-neutron-star matter

J. Roark and V. Dexheimer
Phys. Rev. C 98, 055805 – Published 26 November 2018
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  • INTRODUCTION
  • FORMALISM
  • RESULTS
  • CONCLUSIONS AND OUTLOOK
  • ACKNOWLEDGMENTS
    • References

    Abstract

    In this work, we study in detail the deconfinement phase transition that takes place in hot/dense nuclear matter in the context of neutron stars and proto-neutron stars (in which lepton fraction is fixed). The possibility of different mixtures of phases with different locally and globally conserved quantities is considered in each case. For this purpose, the chiral mean field model, an effective relativistic model that includes self-consistent chiral symmetry restoration and deconfinement to quark matter, is employed. Finally, we compare our results with blue results provided by perturbative QCD for different temperatures and conditions.

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    • Received 6 March 2018
    • Revised 11 September 2018

    DOI:https://doi.org/10.1103/PhysRevC.98.055805

    ©2018 American Physical Society

    Physics Subject Headings (PhySH)

    1. Research Areas
    Nuclear astrophysicsNuclear matter in neutron starsNuclear physics of explosive environmentsQCD phase transitions
    Nuclear PhysicsGravitation, Cosmology & Astrophysics

    Authors & Affiliations

    J. Roark and V. Dexheimer

    • Department of Physics, Kent State University, Kent, Ohio 44243, USA

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    Vol. 98, Iss. 5 — November 2018

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    Images

    • Figure 1
      Figure 1

      The temperature vs. (modified) chemical potential phase diagram for neutron-star matter with locally conserved electric charge and proto-neutron-star matter with locally conserved electric charge and lepton fraction.

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    • Figure 2
      Figure 2

      The temperature vs. baryon chemical potential phase diagram for neutron-star matter with globally conserved electric charge, proto-neutron-star matter with locally conserved electric charge and globally conserved lepton fraction, and proto-neutron-star matter with globally conserved electric charge and lepton fraction.

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    • Figure 3
      Figure 3

      Charged and lepton chemical potentials for neutron-star and proto-neutron-star matter (all charges conserved locally), shown for two different temperatures.

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    • Figure 4
      Figure 4

      Charged and lepton chemical potentials inside the mixtures of phases in proto-neutron-star matter at zero temperature. Black curves show results for the scenario of locally conserved electric charge and globally conserved lepton fraction and red curves show results for the scenario of globally conserved electric charge and lepton fraction, at T=0.

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    • Figure 5
      Figure 5

      Particle populations for neutron-star matter with locally conserved electric charge, at T=0.

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    • Figure 6
      Figure 6

      Particle populations for proto-neutron-star matter with locally conserved electric charge and lepton fraction, at T=0. The curve for electrons mainly overlaps with the curve of protons.

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    • Figure 7
      Figure 7

      Particle populations for neutron-star matter with globally conserved electric charge, at T=0.

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    • Figure 8
      Figure 8

      Particle populations for proto-neutron-star matter with locally conserved electric charge and globally conserved lepton fraction at, T=0. The curve for electrons mainly overlaps with the curve of protons in the hadronic phase.

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    • Figure 9
      Figure 9

      Particle population curves for proto-neutron-star matter with globally conserved electric charge and lepton fraction at, T=0. The curve for electrons mainly overlaps with the curve of protons.

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    • Figure 10
      Figure 10

      Comparison of our results for neutron-star matter (with globally conserved electric charge) with results provided by PQCD, shown for several temperatures (Ref. [32]). Except for the largest temperature, the lower edge of the PQCD regions lie to the right of the figure bounds.

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    • Figure 11
      Figure 11

      Comparison of our results for proto-neutron-star matter (with locally conserved electric charge and globally conserved lepton fraction) with results provided by PQCD, shown for several temperatures (Ref. [32]). Except for the largest temperature, the lower edge of the PQCD regions lie to the right of the figure bounds.

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    • Figure 12
      Figure 12

      The temperature vs. pressure phase diagram for proto-neutron-star matter with locally conserved electric charge and lepton fraction.

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    • Figure 13
      Figure 13

      The temperature vs. number density phase diagram for proto-neutron-star matter with locally conserved electric charge and lepton fraction, locally conserved electric charge and globally conserved lepton fraction, and globally conserved electric charge and lepton fraction.

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    • Figure 14
      Figure 14

      The temperature vs. modified chemical potential phase diagram for proto-neutron-star matter with locally conserved electric charge and lepton fraction. Two example trajectories show the temperature corresponding to a fixed value of entropy density per baryon density (SB=s/nB) for each modified chemical potential.

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