In quasi-free high-energy breakup of a heavy-light bound state, the leading amplitude factors as the product of the remnant light-particle scattering amplitude, a probe-dependent dynamical function, and a real bound-state wavefunction term, with exact unitarity for the remnant subsystem.
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Neutron skin thickness measurements in nuclei, via probes like parity-violating scattering and dipole polarizability, constrain the symmetry energy slope through Bayesian analyses with energy density functionals, linking to neutron star properties.
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Two bodies left behind
In quasi-free high-energy breakup of a heavy-light bound state, the leading amplitude factors as the product of the remnant light-particle scattering amplitude, a probe-dependent dynamical function, and a real bound-state wavefunction term, with exact unitarity for the remnant subsystem.
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Neutron Stars and Neutron Skins: Connecting Finite Nuclei to Dense Matter
Neutron skin thickness measurements in nuclei, via probes like parity-violating scattering and dipole polarizability, constrain the symmetry energy slope through Bayesian analyses with energy density functionals, linking to neutron star properties.