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Massive neutron stars with antikaon condensates in a density-dependent hadron field theory

Prasanta Char and Sarmistha Banik
Phys. Rev. C 90, 015801 – Published 10 July 2014
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  • INTRODUCTION
  • FORMALISM
  • MODEL PARAMETERS
  • RESULTS
  • SUMMARY
  • ACKNOWLEDGEMENTS
    • References

    Abstract

    The measurement of 1.97±0.04Msolar for PSR J1614-2230 and 2.01±0.04Msolar for PSR J0348 + 0432 puts a strong constraint on the neutron star equation of state and its exotic composition at higher densities. In this paper, we investigate the possibility of an exotic equation of state within the observational mass constraint of 2Msolar in the framework of relativistic mean field model with density-dependent couplings. We particularly study the effect of antikaon condensates in the presence of hyperons on the mass-radius relationship of the neutron star.

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    • Received 14 April 2014
    • Revised 16 June 2014

    DOI:https://doi.org/10.1103/PhysRevC.90.015801

    ©2014 American Physical Society

    Authors & Affiliations

    Prasanta Char1 and Sarmistha Banik2

    • 1Astroparticle Physics & Cosmology Division, Saha Institute of Nuclear Physics, 1/AF Bidhannagar, Kolkata 700 064, India
    • 2BITS Pilani, Hyderabad Campus, Samirpet Mondal, Hyderabad 500078, India

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    Issue

    Vol. 90, Iss. 1 — July 2014

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    Images

    • Figure 1
      Figure 1

      Fraction of various particles in β-equlibrated n, p, Λ, and lepton matter including K− and K¯0 condensates for UK¯(n0)=−120 MeV as a function of normalized baryon density.

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    • Figure 2
      Figure 2

      Fraction of various particles in β-equlibrated n, p, Λ, Ξ−, Ξ0, and lepton matter including K− and K¯0 condensates for UK¯(n0)=−120 MeV and −140 MeV as a function of normalized baryon density.

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    • Figure 3
      Figure 3

      The equation of state (EoS), pressure (P) vs energy density (ε). The full line is for n, p, and lepton matter whereas others are with additional K− and K¯0 condensates calculated with UK¯(n0)=−60,−80,−100,−120, and −140 MeV. Deeper UK¯ corresponds to softer EoS.

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    • Figure 4
      Figure 4

      The equation of state (EoS), pressure (P) vs energy density (ε) for various particle combination of n, p, Λ, Ξ−, Ξ0, and lepton in β-equilibrated matter including K− and K¯0 condensates with UK¯(n0)=−120 MeV.

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    • Figure 5
      Figure 5

      The neutron star mass sequences are plotted with radius for the equations of state of Fig. 3. The full line is for n, p, and lepton matter whereas others are with additional K− and K¯0 condensates calculated with UK¯(n0)=−60,−80,−100,−120, and −140 MeV. Deeper UK¯ corresponds to lower line. The gray band specifies the observational limits.

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    • Figure 6
      Figure 6

      The neutron star mass sequences are plotted with radius for the equations of state of Fig. 4. The gray band specifies the observational limits.

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