Abstract
Auxiliary Field Diffusion Monte Carlo (AFDMC) calculations have been employed to revise the interaction beween A-hyperons and nucleons in hypernuclei. The scheme used to describe the interaction, inspired by the phenomenological Argonne-Urbana forces, is the ΛN + ΛNN potential firstly introduced by Bodmer, Usmani et al. Within this framework, we performed calculations on light and medium mass hypernuclei in order to assess the extent of the repulsive contribution of the three-body part. By tuning this contribution in order to reproduce the Λ separation energy in 5ΛHe and 17ΛO, experimental findings are reproduced over a wide range of masses. Calculations have then been extended to Λ-neutron matter in order to derive an analogous of the symmetry energy to be used in determining the equation of state of matter in the typical conditions found in the inner core of neutron stars.
Highlights
The composition of the inner core of neutron stars (NS) still remains a largely unsolved question
The key point of this work is to begin the journey towards an accurate phenomenological hyperon-nucleon interaction that can be employed in many-body Quantum
Given that at present the number and quality of available scattering data do not allow for a substantial improvement of the ΛN contribution, we focused on refitting the coefficients appearing in the three-body ΛN N term
Summary
The composition of the inner core of neutron stars (NS) still remains a largely unsolved question. The fairly recent observation of neutron stars with masses of order 2M [1, 2] has set a rather strong constraint on the stiffness of the equation of state (EoS) of hadronic matter at high densities. On the other hand simple physical arguments can be made, that introduce mechanisms for softening the EoS at high densities. The larger mass of these hadrons (mΣ 1193 MeV and mΛ 1116 MeV), together with the fact that they become distinguishable with respect to nucleons, lowers the energy of the system, making the EoS softer. The softening of the EoS is such that the predicted maximum mass of a NS is not compatible with the current observational data
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
