Domenico Logoteta

Estimation of the effect of hyperonic three-body forces on the maximum mass of neutron stars

A model based on a microscopic Brueckner-Hartree-Fock approach of hyperonic matter supplemented with additional simple phenomenological density-dependent contact terms is employed to estimate the effect of hyperonic three-body forces on the maximum mass of neutron stars. Our results show that although hyperonic three-body forces can reconcile the maximum mass of hyperonic stars with the current limit of 1.4–1.5M⊙, they are unable to provide the repulsion needed to make the maximum mass compatible with the observation of massive neutron stars, such as the recent measurements of the unusually high masses of the millisecond pulsars PSR J1614-2230 (1.97±0.04M⊙) and PSR J1903+0327 (1.667±0.021M⊙).

Quark matter nucleation in hot hadronic matter

Abstract We study the quark deconfinement phase transition in hot β -stable hadronic matter. Assuming a first order phase transition, we calculate the enthalpy per baryon of the hadron–quark phase transition. We calculate and compare the nucleation rate and the nucleation time due to thermal and quantum nucleation mechanisms. We compute the crossover temperature above which thermal nucleation dominates the finite temperature quantum nucleation mechanism. We next discuss the consequences for the physics of proto-neutron stars. We introduce the concept of limiting conversion temperature and critical mass M cr for proto-hadronic stars, and we show that proto-hadronic stars with a mass M M cr could survive the early stages of their evolution without decaying to a quark star.

Quark deconfinement transition in neutron stars with the field correlator method

A phase of strong interacting matter with deconfined quarks is expected in the core of massive neutron stars. In this article, we perform a study of the hadron-quark phase transition in cold (T ¼ 0) neutron star matter and we calculate various structural properties of hybrid stars. For the quark phase, we make use of an equation of state (EOS) derived with the field correlator method (FCM) recently extended to the case of nonzero baryon density. For the hadronic phase, we consider both pure nucleonic and hyperonic matter, and we derive the corresponding EOS within a relativistic mean field approach. We make use of measured

A link between measured neutron star masses and lattice QCD data

We study the hadron-quark phase transition in neutron star matter and the structural properties of hybrid stars using an equation of state (EOS) for the quark phase derived with the field correlator method (FCM). We make use of the measured neutron star masses, and particularly the mass of PSR J1614-2230, to constrain the values of the gluon condensate

Quark matter nucleation in neutron stars and astrophysical implications

G_2

Effects of quark matter nucleation on the evolution of proto-neutron stars

which is one of the EOS parameter within the FCM. We find that the values of

Nuclear matter properties from local chiral interactions with Delta isobar intermediate states

G_2

Chiral model approach to quark matter nucleation in neutron stars

extracted from the mass measurement of PSR J1614-2230 are fully consistent with the values of the same quantity derived, within the FCM, from recent lattice quantum chromodynamics (QCD) calculations of the deconfinement transition temperature at zero baryon chemical potential. The FCM thus provides a powerful tool to link numerical calculations of QCD on a space-time lattice with neutron stars physics.

Millisecond radio pulsars with known masses: Parameter values and equation of state models

Abstract.A phase of strong interacting matter with deconfined quarks is expected in the core of massive neutron stars. We investigate the quark deconfinement phase transition in cold (

Effect of hyperonic three-body forces on the maximum mass of neutron stars

T=0