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PCP(BSK24)

Abstract

This table corresponds to the zero temperature unified equation of state (EoS) for cold non-accreting neutron stars in beta equilibrium based on the Brussels-Montreal energy- density functional BSk24 [GCP_2013]. Details on the EoS model can be found in Ref. [PCP_2018] and the routines to construct an analytical fit of the EoS are also available on the Ioffe website. The tidal deformability associated to this EoS model was calculated in Ref. [ PCS_2019]. The outer crust was calculated using the Hartree-Fock-Bogoliubov atomic mass table HFB-24 available on the BRUSLIB data base [ XGJCA_2013], except when experimental values were available, for which we used the 2016 Atomic Mass Evaluation [ WGKH_2016], supplemented by the measurements of copper isotopes from Ref. [ W_2017]. The inner crust was computed using the 4th-order Extended Thomas-Fermi (ETF) method with proton shell and pairing corrections added perturbatively via the Strutinsky integral (SI); the nucleon distributions were parametrized using damped Fermi profiles and the Coulomb energy was calculated within the Wigner-Seitz (WS) approximation. Although the EoS was originally calculated ignoring nuclear pastas, their presence in neutron-star crust was later discussed in Refs. [ PCP_2020, PC_2022] and was shown to be marginal in the Extended Thomas-Fermi plus Strutinski Integral framework [ PC_2022]. The core was assumed to be made up by an admixture of neutrons and protons neutralised by electrons and possibly by muons. ^1S_0 neutron and proton pairing gaps in neutron-star cores were calculated in Ref. [ AC_2021].

Nparam = 1
Particles = npemN
T min = 0.0
T max = 0.0
T pts = 1
nb min = 4.68e-10
nb max = 1.49e+00
nb pts = 454
Y min = 0.0
Y max = 0.0
Y pts = 1

Nuclear Matter Properties

ns = 0.1578 fm-3
E0 = 16.048 Mev
K = 245.5 Mev
K' = 274.5 Mev
J = 30.0 Mev
L = 46.4 Mev
Ksym = -37.6 MeV

Neutron Star Properties

Mmax = 2.28 Msun
MDU,e = 1.595 Msun
RMmax = 11.08 km
R1.4 = 12.57 km

References

References to the original work:
[WGKH_2016]   M. Wang, G. Audi, F. G. Kondev, W. J. Huang, S. Naimi, and X. Xu, Chinese Physics C41, 030003 (2017)
[AC_2021]   V. Allard and N. Chamel, Universe 7, 470 (2021)
[PC_2022]   J. M. Pearson and N. Chamel, Phys. Rev. C 105, 015803 (2022)
[PCP_2020]   J. M. Pearson, N. Chamel, and A. Y. Potekhin, Phys. Rev. C 101, 015802 (2020)
[PCP_2018]   J. M. Pearson, N. Chamel, A. Y. Potekhin, A. F. Fantina, C. Ducoin, A. K. Dutta, and S. Goriely, MNRAS 481, 2994 (2018)
[GCP_2013]   S. Goriely, N. Chamel, and J. M. Pearson, Phys. Rev. C 88, 024308 (2013)
[PCS_2019]   L. Perot, N. Chamel, and A. Sourie, Phys. Rev. C 100, 035801 (2019)
[XGJCA_2013]   Y. Xu, S. Goriely, A. Jorissen, G. L. Chen, and M. Arnould, Astronomy & Astrophysics 549, A106 (2013)
[W_2017]   A. Welker, et al, Phys. Rev. Lett. 119, 192502 (2017)

Data sheet

eos.pdf

Data

eos.zip (0.17 MB)
eos.zip_checksum.txt
Single files
eos.t
eos.nb
eos.yq
eos.compo
eos.thermo
eos.mr
eos.init
eos.micro
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