Constraining the neutron–proton effective mass splitting using empirical constraints on the density dependence of nuclear symmetry energy around normal density
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Abstract According to the Hugenholtz–Van Hove theorem, nuclear symmetry energy E sym ( ρ ) and its slope L ( ρ ) at an arbitrary density ρ are determined by the nucleon isovector (symmetry) potential U sym ( ρ , k ) and its momentum dependence ∂ U sym ∂ k . The latter determines uniquely the neutron–proton effective k-mass splitting m n − p ⁎ ( ρ , δ ) ≡ ( m n ⁎ − m p ⁎ ) / m in neutron-rich nucleonic matter of isospin asymmetry δ. Using currently available constraints on the E sym ( ρ 0 ) and L ( ρ 0 ) at normal density ρ 0 of nuclear matter from 28 recent analyses of various terrestrial nuclear laboratory experiments and astrophysical observations, we try to infer the corresponding neutron–proton effective k-mass splitting m n − p ⁎ ( ρ 0 , δ ) . While the mean values of the m n − p ⁎ ( ρ 0 , δ ) obtained from most of the studies are remarkably consistent with each other and scatter very closely around an empirical value of m n − p ⁎ ( ρ 0 , δ ) = 0.27 ⋅ δ , it is currently not possible to scientifically state surely that the m n − p ⁎ ( ρ 0 , δ ) is positive within the present knowledge of the uncertainties. Quantifying, better understanding and then further reducing the uncertainties using modern statistical and computational techniques in extracting the E sym ( ρ 0 ) and L ( ρ 0 ) from analyzing the experimental data are much needed.
Subfields: Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/0eafeb17cf6c77f69c998f9eeba0ed32dd2c55e0
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In Nuclear and High Energy Physics
Citations in the corpus
- Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817 (2021, background): “For these demonstrations, the magnitude S ≈ 32± 4 MeV and slope L ≈ 60± 30 MeV of symmetry energy at ρ0 [54], the incompressibility K0 ≈ 240 ± 40 MeV [164–168], skewness J0 ≈ −300 ± 200 MeV [169], and and kurtosis I0 ≈ 0± 2000 MeV of SNM were adopted in Reference [53].”
- Combined Constraints on the Equation of State of Dense Neutron-rich Matter from Terrestrial Nuclear Experiments and Observations of Neutron Stars (2018, background): “(Danielewicz et al. 2002; Shlomo et al. 2006; Chen et al. 2009; Steiner et al. 2010; Piekarewicz 2010; Khan et al. 2012; Dutra et al. 2012, 2014; Li & Han 2013; Colò et al. 2014; Cai & Chen 2014; Zhang et al. 2017).”
- The Nuclear Symmetry Energy (2016, methodology): “This conclusion is in contradiction with the analyses reported in ref.[200], where the current data on Esym(ρ0) and L(ρ0), as derived from various terrestrial nuclear laboratory experiments and astrophysical observations, were used to put constraints on the effective mass splitting.”