The most accurate approach to determine the compressibility of nuclear matter remains the one based on microscopic energy density functionals (EDFs). Recent analyses yield a value for nuclear incompressibility modulus $K_{\mathrm{sat}}=240\pm 20\mathrm{MeV}$, defined in nuclear matter as the second derivative of the energy per particle at saturation density. However, we demonstrate that the compressibility modulus can be reduced to values shifted by four times the suggested uncertainty, i.e., $K_{\mathrm{sat}}\approx 160\mathrm{MeV}$, by providing examples based on models where the second derivative ($K_{\mathrm{sat}}$) and third derivative ($Q_{\mathrm{sat}}$) of the energy per particle at saturation density can be independently varied, while the experimental binding energies, charge radii, and isoscalar giant monopole resonance data in ${}^{120}\mathrm{Sn}$ and ${}^{208}\mathrm{Pb}$ are enforced. The present work suggests a new methodology to access the compressibility of nuclear matter from nuclear experiments, still based on microscopic models, but using EDFs containing more flexibility than the ones employed up to now. Consequences of our results for nuclear matter at suprasaturation density are also discussed by exploring the quarkyonic crossover. We predict that, for our models with low values for $K_{\mathrm{sat}}$, the quark onset density has to be low for neutron stars to exist.

Close

PrevNext

View figure in article

• Collective models
• Equations of state of nuclear matter
• Gravitational waves
• Nuclear astrophysics
• Nuclear density functional theory
• Nuclear forces
• Nuclear matter in neutron stars
• Nucleon-nucleon interactions