Mario Centelles

TL;DR: In this article, a new equation of state for the nucleonic and hyperonic inner core of neutron stars is obtained from a new parametrization of the FSU2 relativistic mean field functional that satisfies these latest astrophysical constraints and reproduces the properties of nuclear matter and finite nuclei while fulfilling the restrictions on high-density matter deduced from heavy-ion collisions.

TL;DR: In this article, the authors re-examine the equation of state for the nucleonic and hyperonic inner core of neutron stars that satisfies the 2M⊙ observations as well as the recent determinations of stellar radii below 13 km, while fulfilling the saturation properties of nuclear matter and finite nuclei together with the constraints on the high density nuclear pressure coming from heavy-ion collisions.

TL;DR: In 2018, Treballs Finals de Grau de Fisica as mentioned in this paper were held at the Universitat de Barcelona, Spain, Curs: 2018, Tutora: Angels Ramos

TL;DR: In this paper, cooling simulations for isolated neutron stars using recently developed equations of state for their core are obtained from new parametrizations of the FSU2 relativistic mean-field functional that reproduce the properties of nuclear matter and finite nuclei, while fulfilling the restrictions on high-density matter deduced from heavy-ion collisions.

TL;DR: In this paper, the authors reexamine the equation of state for the nucleonic and hyperonic inner core of neutron stars that satisfies the 2$M{\odot}$ observations as well as the recent determinations of stellar radii below 13 km, while fulfilling the saturation properties of nuclear matter and finite nuclei together with the constraints on the high density nuclear pressure coming from heavy-ion collisions.