Constança Providência

Quark matter under strong magnetic fields in the su(3) Nambu-Jona-Lasinio model

D.P. Menezes, M. Benghi Pinto, S.S. Avancini, A. Pérez Mart́ınez, and C. Providência Depto de F́ısica CFM Universidade Federal de Santa Catarina Florianópolis SC CP. 476 CEP 88.040 900 Brazil Instituto de Cibernética Matemática y F́ısica (ICIMAF) Calle E esq 15 No. 309 Vedado, Havana, 10400, Cuba Centro de F́ısica Computacional Department of Physics University of Coimbra P-3004 516 Coimbra Portugal

Relativistic Mean-Field Hadronic Models under Nuclear Matter Constraints

Relativistic mean-field (RMF) models have been widely used in the study of many hadronic frameworks because of several important aspects not always present in nonrelativistic models, such as intrinsic Lorentz covariance, automatic inclusion of spin, appropriate saturation mechanism for nuclear matter, causality and, therefore, no problems related to superluminal speed of sound. With the aim of identifying the models which best satisfy well known properties of nuclear matter, we have analyzed

Inverse magnetic catalysis in the ( 2 + 1 ) -flavor Nambu–Jona-Lasinio and Polyakov–Nambu–Jona-Lasinio models

263

Deconfinement and chiral restoration within the SU(3) Polyakov-Nambu-Jona-Lasinio and entangled Polyakov-Nambu-Jona-Lasinio models in an external magnetic field

parameterizations of seven different types of RMF models under three different sets of constraints related to symmetric nuclear matter, pure neutron matter, symmetry energy, and its derivatives. One of these (SET1) is formed of the same constraints used in a recent work [M. Dutra et al., Phys. Rev. C 85, 035201 (2012)] in which we analyzed

Hyperons in neutron star matter within relativistic mean-field models

240

Nuclear symmetry energy and the role of the tensor force

Skyrme parameterizations. The results pointed to

Quark-hadron phase transition in a neutron star under strong magnetic fields

2

Neutron star radii and crusts: Uncertainties and unified equations of state

models consistent with all constraints. By using another set of constraints, namely, SET2a, formed by the updated versions of the previous one, we found

Core-crust transition in neutron stars: Predictivity of density developments

4

Warm stellar matter with deconfinement: Application to compact stars

models approved simultaneously. Finally, in the third set, named SET2b, in which the values of the constraints are more restrictive, we found