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
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 |