Feasibility study of a dark matter admixed neutron star based on recent observational constraints

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Table A.1.

Empirical constraints from experimental and observational data.

Symmetric matter
Constraints	n (fm⁻³)	P_SNM (MeV/fm³)		Ref.
HIC(DLL)	0.32	10.1 ± 3.0		Danielewicz et al. (2002)
HIC(FOPI)	0.32	10.3 ± 2.8		Le Fèvre et al. (2016)

Asymmetric matter
Constraints	n (fm⁻³)	e_sym (MeV)	P_sym (MeV/fm³)	Ref.

Nuclear structure
α_D	0.05	15.9 ± 1.0		Zhang & Chen (2015)
PREX-II	0.11		2.38 ± 0.75	Adhikari et al. (2021), Reed et al. (2021), Lynch & Tsang (2022)
Nuclear masses
Mass(Skyrme)	0.101	24.7 ± 0.8		Brown & Schwenk (2014), Lynch & Tsang (2022)
Mass(DFT)	0.115	25.4 ± 1.1		Kortelainen et al. (2012), Lynch & Tsang (2022)
IAS	0.106	25.5 ± 1.1		Danielewicz et al. (2017), Lynch & Tsang (2022)
Heavy-ion collisions
HIC(Isodiff)	0.035	10.3 ± 1.0		Tsang et al. (2009), Lynch & Tsang (2022)
HIC(n/p ratio)	0.069	16.8 ± 1.2		Morfouace et al. (2019), Lynch & Tsang (2022)
HIC(π)	0.232	52 ± 13	10.9 ± 8.7	Estee et al. (2021), Lynch & Tsang (2022)
HIC(n/p flow)	0.240		12.1 ± 8.4	Cozma (2018), Russotto et al. (2011, 2016), Lynch & Tsang (2022)

Astrophysical
Constraints	M_⊙	R (km)	Λ_1.36	Ref.

LIGO ¹	1.36		$300_{- 230}^{+ 420}$ $300_{-230}^{+420}$	Abbott et al. (2019)
Riley PSR J0030+0451 ²	1.34	$12 . 71_{- 1.19}^{+ 1.14}$ $12.71^{+1.14}_{-1.19}$		Riley et al. (2019)
Miller PSR J0030+0451 ³	1.44	$13 . 02_{- 1.06}^{+ 1.24}$ $13.02^{+1.24}_{-1.06}$		Miller et al. (2019)
Riley PSR J0740+6620 ⁴	2.07	12.39 $_{- 0.98}^{+ 1.30}$ $^{+1.30}_{-0.98}$		Riley et al. (2021)
Miller PSR J0740+6620 ⁵	2.08	$13.7_{- 1.5}^{+ 2.6}$ $13.7~^{+2.6}_{-1.5}$		Miller et al. (2021)
Choudhury PSR J0437-4715 ⁶	1.418	$11.36_{- 0.63}^{+ 0.95}$ $11.36~^{+0.95}_{-0.63}$		Choudhury et al. (2024)

Notes. This table presents empirical values of symmetry energy (e_sym), symmetry energy pressure (P_sym), and symmetric nuclear matter pressure (P_SNM) from experimental data on the bulk properties of finite nuclei and HIC. The astrophysical observational constraints on the radii and tidal deformability of neutron stars are also included. See Ref Tsang et al. (2024) for details.

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