The formalism of nuclear many-body theory can be exploited to carry out accurate calculations of a variety of nuclear properties relevant to the understanding of fundamental physics issues under active experimental investigation.

The CBF effective interaction has been first employed to evaluate the in-medium nucleon-nucleon scattering cross section. The results of this calculation were then used to obtain the shear viscosity of pure neutron matter within the formalism of Landau, Abrikosov and Khalatnikov [Phys. Rev. Lett. 99 (2007) 232501]. The understanding of this property is essential to determine the onset of the Chandrasekhar-Friedman-Schutz (CFS) instability, driven by gravitational wave emission, in rapidly rotating stars.

The nuclear matter equation of state (EOS) has been shown to appreciably affect gravitational wave emission from compact stars [Phys. Rev. D 70 (2004) 124015]. The detection of gravitational waves is, in fact, expected to resolve the large degree of degeneracy of the models employed to obtain the EOS of neutron star matter, thus ushering a new era of gravitational wave asteroseismology.

A significant contribution towards the understanding of the EOS of matter in the interior of neutron stars may also come from measurements of their thermal evolution. In this context, I have studied the possible occurrence of a superfluid phase in the inner crust [J. Low. Temp. Phys. 189 (2017) 250], which is known to play an important role.

The ongoing experimental studies of neutrinoless double-β decay, aimed at determining whether the neutrino is a Dirac or Majorana fermion, rely on highly non trivial theoretical calculations of the nuclear transition matrix element. The role of correlations in this context does not appear to be fully under control yet, and accurate consistent calculations carried out within the CBF approach may provide much needed additional information [Phys. Rev. C 90 (2014) 093004].