Bruno Franzon

Effects of strong magnetic fields and rotation on white dwarf structure

In this work we compute models for relativistic white dwarfs in the presence of strong magnetic fields. These models possibly contribute to super-luminous SNIa. With an assumed axi-symmetric and poloidal magnetic field, we study the possibility of existence of super-Chandrasekhar magnetized white dwarfs by solving numerically the Einstein-Maxwell equations, by means of a pseudo-spectral method. We obtain a self-consistent rotating and non-rotating magnetized white dwarf models. According to our results, a maximum mass for a static magnetized white dwarf is 2.13

The internal composition of proto-neutron stars under strong magnetic fields

\rm{M_{\odot}}

Many-body Forces in Magnetic Neutron Stars

in the Newtonian case and 2.09

A self-consistent study of magnetic field effects on hybrid stars

\rm{M_{\odot}}

White Dwarf Pulsars and Very Massive Compact Ultra Magnetized White Dwarfs

while taking into account general relativistic effects. Furthermore, we present results for rotating magnetized white dwarfs. The maximum magnetic field strength reached at the center of white dwarfs is of the order of

Effects of magnetic fields in white dwarfs

10^{15}\,

The population of highly magnetized neutron stars

G in the static case, whereas for magnetized white dwarfs, rotating with the Keplerian angular velocity, is of the order of

Highly Magnetized Neutron Stars in a Many-body Forces Formalism

10^{14}\,

Effects of strong magnetic fields on hybrid stars

G.

Effects of the quark-hadron phase transition on highly magnetized neutron stars

In this work, we study the effects of magnetic fields and rotation on the structure and composition of proto-neutron stars. A hadronic chiral SU(3) model is applied to cold neutron stars and proto-neutron stars with trapped neutrinos and at fixed entropy per baryon. We obtain general relativistic solutions for neutron and proto-neutron stars endowed with a poloidal magnetic field by solving Einstein-Maxwell field equations in a self-consistent way. As the neutrino chemical potential decreases in value over time, this alters the chemical equilibrium and the composition inside the star, leading to a change in the structure and in the particle population of these objects. We find that the magnetic field deforms the star and significantly alters the number of trapped neutrinos in the stellar interior, together with strangeness content and temperature in each evolution stage.