New ab initio constrained extended Skyrme equations of state for simulations of neutron stars, supernovae, and binary mergers - I. Subsaturation density domain

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Table 2.

Values of selected NM parameters corresponding to the effective interactions in Table 1.

Param.	Units	BBSk1	BBSk2	BBSk3	BBSk4	BBSk5
n_sat	fm⁻³	0.161	0.154	0.165	0.164	0.158
E_sat	MeV	−15.75	−15.78	−15.98	−15.71	−15.78
K_sat	MeV	243	287	225	248	228
Q_sat	MeV	−378	−271	−452	−369	−327
Z_sat	MeV	1486	362	2084	1364	1633
J_sym	MeV	30.9	31.4	29.6	30.1	32.8
L_sym	MeV	52.6	55.4	39.6	56.8	61.3
K_sym	MeV	−118	−146	−146	−55	−126
Q_sym	MeV	471	323	649	541	270
Z_sym	MeV	−2103	−1339	−2526	−2677	−1615
m_eff; N^SNM	m_N	0.630	0.818	0.461	0.422	0.940
m_eff; n^PNM	m_n	0.852	0.965	0.725	0.747	0.979
T_C	MeV	17.21	17.28	18.23	19.38	15.84

Notes. Provided are the saturation density (n_sat) of the SNM; the energy per nucleon (E_sat), compression modulus (K_sat), skewness (Q_sat), and kurtosis (Z_sat) of the SNM at n_sat; the critical temperature (T_C) for the liquid gas phase transition of the SNM; the symmetry energy (J_sym), its slope (L_sym), compressibility (K_sym), skewness (Q_sym), and kurtosis (Z_sym) at n_sat; and the Landau effective mass of the nucleons in the SNM (m_eff; N^SNM) and the Landau effective mass of the neutrons in the PNM (m_eff; n^PNM) at 0.16 fm⁻³.

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