Diego Lonardoni

Accurate determination of the interaction between Λ hyperons and nucleons from auxiliary field diffusion Monte Carlo calculations

Background: An accurate assessment of the hyperon-nucleon interaction is of great interest in view of recent observations of very massive neutron stars. The challenge is to build a realistic interaction that can be used over a wide range of masses and in infinite matter starting from the available experimental data on the binding energy of light hypernuclei. To this end, accurate calculations of the hyperon binding energy in a hypernucleus are necessary.

Effects of the two-body and three-body hyperon-nucleon interactions in Λ hypernuclei

Background: The calculation of the hyperon binding energy in hypernuclei is crucial to understanding the interaction between hyperons and nucleons.

Variational Calculation of the Ground State of Closed-Shell Nuclei Up to

Variational calculations of ground-state properties of

A

^4

= 40

He,

From hypernuclei to the inner core of neutron stars: A quantum Monte Carlo study

^{16}

Auxiliary field diffusion Monte Carlo calculations of light and medium-mass nuclei with local chiral interactions

O, and

The EOS of neutron matter, and the effect of Lambda hyperons to neutron star structure

^{40}

Recent progress on the accurate determination of the equation of state of neutron and nuclear matter

Ca are carried out employing realistic phenomenological two- and three-nucleon potentials. The trial wave function includes two- and three-body correlations acting on a product of single-particle determinants. Expectation values are evaluated with a cluster expansion for the spin-isospin dependent correlations considering up to five-body cluster terms. The optimal wave function is obtained by minimizing the energy expectation value over a set of up to 20 parameters by means of a nonlinear optimization library. We present results for the binding energy, charge radius, one- and two-body densities, single-nucleon momentum distribution, charge form factor, and Coulomb sum rule. We find that the employed three-nucleon interaction becomes repulsive for

Exotic atoms at extremely high magnetic fields: the case of neutron star atmosphere

A\geq16