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It has been recently suggested that differences in the charge radii of mirrornuclei are proportional to the neutron-skin thickness of neutron-rich nucleiand to the slope of the symmetry energy $L$ [B.A. Brown Phys. Rev. Lett. 119,122502 (2017)]. The determination of the neutron skin has importantimplications for nuclear physics and astrophysics. Although the use ofelectroweak probes provides a largely model-independent determination of theneutron skin, the experimental challenges are enormous. Thus, the possibilitythat differences in the charge radii of mirror nuclei may be used as asurrogate for the neutron skin is a welcome alternative. To test the validityof this assumption we perform calculations based on a set of relativisticenergy density functionals that span a wide region of values of $L$. Ourresults confirm that the difference in charge radii of variousneutron-deficient nickel isotopes and their corresponding mirror nuclei isindeed 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 ofmirror nuclei and the radius of low-mass neutron stars.

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