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ABHT(QMC-RMF4)

Abstract

An EoS in β-equilibrium at T = 0. The core is homogeneous n, p, e matter that begins above 0.10 fm^−3. It is computed using a relativistic mean-field theory constrained by chiral effective field theory calculations of pure neutron matter (from 0.08 fm^−3 to 0.32 fm^−3) and by properties of isospin-symmetric nuclear matter around saturation density [ABHT_2022 ]. The outer crust is the Baym-Pethick-Sutherland (BPS) EoS and spans the density range 6.30 × 10^−12 fm^−3 to 2.57 × 10^−4 fm^−3 [BPSA_1971]. The inner crust is the GPPVA(TM1e) EoS, which models nuclear pasta phases calculated within a self-consistent Thomas- Fermi approach from 2.00 × 10^−3 fm^−3 to 6.24 × 10^−2 fm^−3 [GPPVP_2014]. A first-order phase transition to the core is imposed at a baryon chemical potential of 952.22 MeV.

Nparam = 1
Particles = npeN
T min = 0.0
T max = 0.0
T pts = 1
nb min = 6.30e-11
nb max = 1.36e+00
nb pts = 301
Y min = 0.0
Y max = 0.0
Y pts = 1

Nuclear Matter Properties

ns = 0.162 fm-3
E0 = -16.1 Mev
K = 279.0 Mev
K' = 311.0 Mev
J = 30.4 Mev
L = 31.3 Mev
Ksym = -54.0 MeV

Neutron Star Properties

Mmax = 2.21 Msun
MDU,e = N/A Msun
RMmax = 11.03 km
R1.4 = 12.35 km

References

References to the original work:
[GPPVP_2014]   F. Grill, H. Pais, C. Providencia, I. Vidana and S. S. Avancini, Phys. Rev. C 90, 045803 (2014)
[BPSA_1971]   G. Baym, C. Pethick and P. Sutherland, Astrophys. J. 170, 299 (1971)
[ABHT_2022]   M. G. Alford, L. Brodie, A. Haber, and I. Tews, Phys. Rev. C 106, 055804 (2022)

Data sheet

eos.pdf

Data

eos.zip (0.15 MB)
eos.zip_checksum.txt
Single files
eos.mr
eos.compo
eos.init
eos.micro
eos.thermo
eos.t
eos.nb
eos.yq
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