Constant entropy hybrid stars: a first approximation of cooling evolution

Abstract

Aims. We aim to study the possibility of a hadron-quark phase transition in the interior of neutron stars, taking into account different schematic evolutionary stages at finite temperature. We also discuss the strange quark matter stability in the quark matter phase.Furthermore, we aim to analyze the astrophysical properties of hot and cold hybrid stars, considering the constraint on maximum mass given by the pulsars J1614-2230 and J0348+0432. Methods. We have developed a computational code to construct semi-analytical hybrid equations of state at fixed entropy per baryon and to obtain different families of hybrid stars. An analytical approximation of the Field Correlator Method is developed for the quark matter equation of state. For the hadronic equation of state we use a table based on the relativistic mean field theory, without hyperons. The phase transition was obtained imposing the Maxwell conditions, by assuming a high surface tension at the interface hadron-quark. We solved the relativistic structure equations of hydrostatic equilibrium and mass conservation for hybrid star configurations. Results. For the different equations of state obtained, we calculated the stability window for the strange quark matter, lepton abundances, temperature profiles and contours profiles for the maximum mass star depending on the parameters of the Field Correlator Method. We also computed the mass-radius and gravitational mass-baryonic mass relationships for different hybrid star families. Conclusions. We have analyzed different stages of hot hybrid stars as a first approximation of the cooling evolution of neutron stars with quark matter cores. We obtain cold hybrid stars with maximum masses ≥ 2M for different combinations of the Field Correlator Method parameters. In addition, our study based on the gravitational mass -baryonic mass plane shows a late phase transition between hadronic and quark matter during the proto-hybrid star evolution, in contrast with previous studies of proto-neutron stars.

Magnetized hybrid stars: effects of slow and rapid phase transitions at the quark–hadron interface

“…In this work, we will analyse in detail the structure and stability of low-B HSs and magnetars under rapid and slow phase conversions. Besides, we will analyse the gravitational mass versus baryon mass diagram to estimate the energy released when a magnetar evolves to become a low-B object, based on the ideas developed in Bombaci (1996) and already presented in Mariani et al (2017).…”

“…In order to automate the calculations and integrate the whole process, we use the multi-language NeStOR code introduced in Mariani et al (2017). Originally developed to construct EoS at finite temperature and calculate the structure of proto-NS, we adapted the code to run the magnetised EoS codes and implemented a procedure to detect the change of stability of radial oscillation modes.…”

Thermodynamic potential for quark-qluon plasma with finite quark mass and chemical potential

“…Hence, we do not describe the critical point deduced from LGT, but take that as a given. Moreover, the order of the transition requires a determination of the surface tension for nucleated bubbles of QGP [2,18]. However, there is considerable uncertainty in the surface tension.…”

“…However, there is considerable uncertainty in the surface tension. Hence, we assume an abrupt transition between hadronic and quark matter as in [18].…”

Simplified Thermal Evolution of Proto-Hybrid Stars

“…7 ). In the NS regime of low temperature and high densities, bottom part of the orange shaded region in Fig.…”