We study the influence of core-crust transition pressure changes on the general dynamical properties of neutron star configurations. First we study the matching conditions in core-crust transition pressure region, where phase transitions in the equation of state causes energy density jumps. Then using a surface crust approximation, we can construct configurations where the matter is described by the equation of state of the core of the star and the core-crust transition pressure. We will consider neutron stars in the slow rotation limit, considering perturbation theory up to second order in the angular velocity so that the deformation of the star is also taken into account. The junction determines the parameters of the star such as total ma...
International audienceThe crust-core (CC) phase transition of neutron stars is studied within a unif...
Journals published by the American Physical Society can be found at http://publish.aps.org/Using the...
Aims.We analyze potentially observable phenomena during spin evolution of isolated pulsars, such as ...
Introducing a surface layer of matter on the edge of a neutron star in slow rigid rotation, we analy...
The transition density nt and pressure Pt at the inner edge between the liquid core and the solid cr...
As a rapidly rotating neutron star spins down due to the loss of its angular momentum, its central d...
Aims. We calculate parameters A and B of the Baym-Pines model of the hydro-elastic equilibrium of ro...
As a rapidly rotating neutron star spins down due to the loss of its angular momentum, its central d...
The possibility to draw links between the isospin properties of nuclei and the structure of compact ...
International audienceAims: We calculate parameters A and B of the Baym-Pines model of the hydro-ela...
Transitions of nuclear compositions in the crust of a neutron star induced by stellar spin-down are ...
The slope of the nuclear symmetry energy at saturation density $L$ is pointed out as a crucial quant...
In this paper, we have calculated the core-crust transition parameters and the location of inner edg...
The impact of the equation of state (EoS) crust-core matching procedure on neutron star (NS) proper...
We address the issues of crustal properties of neutron stars such as crustal mass, crustal radius, c...
International audienceThe crust-core (CC) phase transition of neutron stars is studied within a unif...
Journals published by the American Physical Society can be found at http://publish.aps.org/Using the...
Aims.We analyze potentially observable phenomena during spin evolution of isolated pulsars, such as ...
Introducing a surface layer of matter on the edge of a neutron star in slow rigid rotation, we analy...
The transition density nt and pressure Pt at the inner edge between the liquid core and the solid cr...
As a rapidly rotating neutron star spins down due to the loss of its angular momentum, its central d...
Aims. We calculate parameters A and B of the Baym-Pines model of the hydro-elastic equilibrium of ro...
As a rapidly rotating neutron star spins down due to the loss of its angular momentum, its central d...
The possibility to draw links between the isospin properties of nuclei and the structure of compact ...
International audienceAims: We calculate parameters A and B of the Baym-Pines model of the hydro-ela...
Transitions of nuclear compositions in the crust of a neutron star induced by stellar spin-down are ...
The slope of the nuclear symmetry energy at saturation density $L$ is pointed out as a crucial quant...
In this paper, we have calculated the core-crust transition parameters and the location of inner edg...
The impact of the equation of state (EoS) crust-core matching procedure on neutron star (NS) proper...
We address the issues of crustal properties of neutron stars such as crustal mass, crustal radius, c...
International audienceThe crust-core (CC) phase transition of neutron stars is studied within a unif...
Journals published by the American Physical Society can be found at http://publish.aps.org/Using the...
Aims.We analyze potentially observable phenomena during spin evolution of isolated pulsars, such as ...