Helena Pais

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

We study the effect of a strong magnetic field on the properties of neutron stars with a quark–hadron phase transition. It is shown that the magnetic field prevents the appearance of a quark phase, enhances the leptonic fraction, decreases the baryonic density extension of the mixed phase and stiffens the total equation of state, including both the stellar matter and the magnetic field contributions. Two parametrizations of a density-dependent static magnetic field, increasing, respectively, fast and slowly with the density and reaching 2–4 × 1018 G in the centre of the star, are considered. The compact stars with strong magnetic fields have maximum mass configurations with larger masses and radii and smaller quark fractions. The parametrization of the magnetic field with density has a strong influence on the star properties.

Equation of state and thickness of the inner crust of neutron stars

The cell structure of

Light clusters, pasta phases and phase transitions in core-collapse supernova matter

\beta

Strong correlations of neutron star radii with the slopes of nuclear matter incompressibility and symmetry energy at saturation

-stable clusters in the inner crust of cold and warm neutron stars is studied within the Thomas-Fermi approach using relativistic mean field nuclear models. The relative size of the inner crust and the pasta phase of neutron stars is calculated, and the effect of the symmetry energy slope parameter,

Correlation of the neutron star crust-core properties with the slope of the symmetry energy and the lead skin thickness

L

Neutron stars: From the inner crust to the core with the (extended) Nambu–Jona-Lasinio model

, on the profile of the neutron star crust is discussed. It is shown that while the size of the total crust is mainly determined by the incompressibility modulus, the relative size of the inner crust depends on

Dynamical properties of nuclear and stellar matter and the symmetry energy

L

Light clusters and pasta phases in warm and dense nuclear matter

. It is found that the inner crust represents a larger fraction of the total crust for smaller values of

Dynamical instabilities of warm npe- matter: The delta meson effects

L

Crust-core transition of a neutron star: Effects of the symmetry energy and temperature under strong magnetic fields

. Finally, it is shown that at finite temperature the pasta phase in