Density slope of the nuclear symmetry energy from the neutron skin thickness of heavy nuclei
By Lie-Wen Chen, C. Ko, Bao-An Li, Jun Xu. 2010
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Expressing explicitly the parameters of the standard Skyrme interaction in terms of the macroscopic properties of asymmetric nuclear matter, we show in the Skyrme-Hartree-Fock approach that unambiguous correlations exist between observables of finite nuclei and nuclear matter properties. We find that existing data on neutron skin thickness $\ensuremath{\Delta}{r}_{\mathit{np}}$ of Sn isotopes give an important constraint on the symmetry energy ${E}_{\mathrm{sym}}({\ensuremath{\rho}}_{0})$ and its density slope $L$ at saturation density ${\ensuremath{\rho}}_{0}$. Combining these constraints with those from recent analyses of isospin diffusion and the double neutron/proton ratio in heavy-ion collisions at intermediate energies leads to a more stringent limit on $L$ approximately independent of ${E}_{\mathrm{sym}}({\ensuremath{\rho}}_{0})$. The implication of these new constraints on the $\ensuremath{\Delta}{r}_{\mathit{np}}$ of $^{208}\mathrm{Pb}$ as well as the core-crust transition density and pressure in neutron stars is discussed.
Subfields: Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/df7f25911fddfffb3bd31d68e41cc67a9d9235f3
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In Nuclear and High Energy Physics
Citations in the corpus
- The Nuclear Symmetry Energy (2016, methodology): “ards, taken from ref. [178]. v) We finally add the constraints from the skin width data, combined with isospin diusion and neutron to proton double ratio in heavy ion collision, as elaborated in ref. [274], see also Sec. 4. This is represented by the (blue) band going downwards. We report also the (y”
- Nuclear equation of state from ground and collective excited state properties of nuclei (2018, background): “Next, in left lower panel of the same figure, constraints from a theoretical analysis on L and J (written as Esym(ρ0) in the figure) from a χ(2) analysis of available data from proton scattering, alpha scattering, and antiprotonic atoms (see Ref.[173] for details) on the neutron skin thickness of so”
- Unified equation of state for neutron stars on a microscopic basis (2015, background): “…values for Esym(n0) and L lie within the recent constraints derived from the analysis of different astrophysical observations (Newton et al. 2013; Steiner et al. 2010; Lattimer & Lim 2013; Hebeler et al. 2013) and nuclear experiments (Chen et al. 2010; Tsang et al. 2012; Viñas et al. 2014).”