Difference in proton radii of mirror nuclei as a possible surrogate for the neutron skin

Abstract

It has been recently suggested that differences in the charge radii of mirror nuclei are proportional to the neutron-skin thickness of neutron-rich nuclei and to the slope of the symmetry energy $L$ [B.A. Brown Phys. Rev. Lett. 119, 122502 (2017)]. The determination of the neutron skin has important implications for nuclear physics and astrophysics. Although the use of electroweak probes provides a largely model-independent determination of the neutron skin, the experimental challenges are enormous. Thus, the possibility that differences in the charge radii of mirror nuclei may be used as a surrogate for the neutron skin is a welcome alternative. To test the validity of this assumption we perform calculations based on a set of relativistic energy density functionals that span a wide region of values of $L$. Our results confirm that the difference in charge radii of various neutron-deficient nickel isotopes and their corresponding mirror nuclei is indeed strongly correlated to both the neutron-skin thickness and $L$. Moreover, given that various neutron-star properties are also sensitive to $L$, a data-to-data relation emerges between the difference in charge radii of mirror nuclei and the radius of low-mass neutron stars.

5 pages, 3 figures

References in corpus (12)

• GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
• Neutron Star Observations: Prognosis for Equation of State Constraints
• Neutron-Rich Nuclei in Heaven and Earth
• Nuclear symmetry energy probed by neutron skin thickness of nuclei
• Neutron skin of 208Pb, nuclear symmetry energy, and the parity radius experiment
• Relativistic effective interaction for nuclei, giant resonances, and neutron stars
• Building relativistic mean field models for finite nuclei and neutron stars
• Core-crust transition in neutron stars: predictivity of density developments
• Pygmy dipole resonance as a constraint on the neutron skin of heavy nuclei
• Pygmy Resonances and Neutron Skins
• Isospin Diffusion in Heavy-Ion Collisions and the Neutron Skin Thickness of Lead
• Pygmy and core polarization dipole modes in ${}^{206}$Pb: connecting nuclear structure to stellar nucleosynthesis

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