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Properties of rapidly rotating hot neutron stars with antikaon condensates at constant entropy per baryon

Neelam Dhanda Batra, Krishna Prakash Nunna, and Sarmistha Banik
Phys. Rev. C 98, 035801 – Published 4 September 2018
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  • INTRODUCTION
  • MODELS OF COMPACT STARS
  • RESULTS
  • CONCLUSIONS
  • ACKNOWLEDGMENTS
    • References

    Abstract

    We consider a neutrino-free hot neutron star that contains antikaon condensates in its core and is at finite entropy per baryon. We find the equation of state for a range of entropies and antikaon optical potentials and generate the mass profile of static as well as rotating stars. Rotation induces many changes in the stellar equilibrium, and hence its structural properties evolve. In this work, we report the effect of rotation on the mass and shape of a hot neutron star for different equations of state and thermodynamic conditions. The temperature profile of a hot, static neutron star is also explored. We also make a crude estimate of the amplitude of gravitational waves emitted by an axisymmetric rotating NS with high magnetic field.

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    • Received 13 June 2017
    • Revised 10 August 2018

    DOI:https://doi.org/10.1103/PhysRevC.98.035801

    ©2018 American Physical Society

    Physics Subject Headings (PhySH)

    1. Research Areas
    Nuclear astrophysicsNuclear matter in neutron stars
    Nuclear Physics

    Authors & Affiliations

    Neelam Dhanda Batra1,2, Krishna Prakash Nunna1, and Sarmistha Banik1

    • 1Department of Physics, BITS Pilani, Hyderabad Campus, Jawahar Nagar, Medchal District-500078, India
    • 2Department of Physics, Indian Institute of Technology, New Delhi-110016, India

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    Issue

    Vol. 98, Iss. 3 — September 2018

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    Images

    • Figure 1
      Figure 1

      (a) The EoS with pressure plotted against number density for np and npK (UK¯=−100MeV) for a NS core at zero temperature state (T=0 MeV) and at adiabatic state (entropy per baryon s=1, 4, and 5). (b) The mass sequences against number densities for the np and npK (UK¯=−100MeV) EoS, for total entropy S=0, 3, 5, and 7 Msolar. The dashed lines are for np matter and solid lines are for npK matter for UK¯=−100 MeV in both the panels.

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    • Figure 2
      Figure 2

      The EoS is plotted for a range of values of UK¯=−60MeV to −150MeV (a) for lower s=1 and (b) for higher s=4. In both the plots np EoS is also included as the dashed line for comparison.

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    • Figure 3
      Figure 3

      The mass-number density profiles for EoS with np and npK matter at different optical potentials at for (a) S=3Msolar and (b) S=7Msolar.

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    • Figure 4
      Figure 4

      Fraction of different particles in a β-equilibrated NS matter with n, p, e, μ, and antikaon condensates of K− and KT; for UK¯=−60 MeV; plotted as a function of the baryon density for (a) s=1 and (b) s=4.

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    • Figure 5
      Figure 5

      Particle fractions vs baryon number density as in Fig 4, but for a deeper UK¯=−150 MeV for (a) s=1 and (b) s=4.

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    • Figure 6
      Figure 6

      Temperature in a NS is plotted as a function of baryon density nb, for a given thermodynamic state, (a) s=1 and (b) s=4.

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    • Figure 7
      Figure 7

      The evolution of mass with rotation for a NS with npK (UK¯=−100MeV) and at (a) S=3Msolar and (b) S=7Msolar. The sequences are plotted for NS rotating with different angular momenta starting from J=0 (static case) to J=1GMsolar2/c and 2GMsolar2/c.

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    • Figure 8
      Figure 8

      Energy density iso-contours of a rotating NS with baryon mass of 2Msolar. Top (bottom) panel shows static NS with EoS for UK¯=−60(−150) MeV, with s=1.

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    • Figure 9
      Figure 9

      Energy density iso-contours of a rotating NS as in Fig. 8, but with higher entropy per baryon state s=4

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    • Figure 10
      Figure 10

      Effect of rotation on NS shape. Energy density iso-contours for a NS with npK (UK¯=−150MeV, s=1) rotating at J=0.02GMsolar2/c (top) and 0.5GMsolar2/c (bottom).

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    • Figure 11
      Figure 11

      Energy density isocontours for a NS as in Fig. 10 rotating at J=1.8GMsolar2/c (top) and 2.23GMsolar2/c (bottom).

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    • Figure 12
      Figure 12

      Fluid energy density isocontours for NS (UK¯=−150 MeV, s=4) rotating at J=0.02GMsolar2/c (top) and at J=1.8GMsolar2/c (bottom).

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