A5003741507- Pulsars and Gravitational Waves Research
- High-pressure geophysics and materials
- Nuclear physics research studies
- Gamma-ray bursts and supernovae
- Quantum, superfluid, helium dynamics
- Geophysics and Gravity Measurements
- Astro and Planetary Science
- Atomic and Subatomic Physics Research
- Astrophysical Phenomena and Observations
- earthquake and tectonic studies
- Nuclear Physics and Applications
- Astronomical and nuclear sciences
- Stellar, planetary, and galactic studies
- Quantum Chromodynamics and Particle Interactions
- Geophysics and Sensor Technology
- Solar and Space Plasma Dynamics
- Geological and Geophysical Studies
- Cosmology and Gravitation Theories
- Cold Atom Physics and Bose-Einstein Condensates
- Atomic and Molecular Physics
- Superconducting Materials and Applications
- Magnetic confinement fusion research
- Astronomical Observations and Instrumentation
- Advanced Chemical Physics Studies
- Earthquake Detection and Analysis
Université Libre de Bruxelles
2016-2025
Chinese University of Hong Kong
2024
Institute of Astronomy
2018
Consejo Superior de Investigaciones Científicas
2016
University of Amsterdam
2016
CEA DAM Île-de-France
2009
Université Paris-Sud
2009
National Superconducting Cyclotron Laboratory
2009
Michigan State University
2009
Johannes Gutenberg University Mainz
2009
We construct three new Hartree-Fock-Bogoliubov (HFB) mass models, labeled HFB-19, HFB-20, and HFB-21, with unconventional Skyrme forces containing ${t}_{4}$ ${t}_{5}$ terms, i.e., density-dependent generalizations of the usual ${t}_{1}$ ${t}_{2}$ respectively. The underlying these models are fitted respectively to different realistic equations state neutron matter for which density dependence symmetry energy ranges from very soft stiff, reflecting thereby our present lack complete knowledge...
We present a new Skyrme-Hartree-Fock-Bogoliubov nuclear-mass model in which the contact-pairing force is constructed from microscopic pairing gaps of symmetric nuclear matter and neutron calculated realistic two- three-body forces, with medium-polarization effects included. With being treated more realistically than any our earlier models, rms deviation respect to essentially all available mass data falls 0.581 MeV, best value ever found within mean-field framework. Since Skyrme also...
Our family of three Hartree-Fock-Bogoliubov (HFB) mass models, labeled BSk19, BSk20, and BSk21, is here extended by (a) refitting to the 2012 Atomic Mass Evaluation (AME), (b) varying symmetry coefficient $J$. Five new BSk22 BSk26, along with their tables, HFB-22 HFB-26, respectively, are presented. These models characterized unconventional Skyrme forces containing ${t}_{4}$ ${t}_{5}$ terms, i.e., density-dependent generalizations usual ${t}_{1}$ ${t}_{2}$ respectively. Highly realistic...
Context. A unified equation of state (EoS) should describe the crust and core a neutron star using same physical model. The Brussels-Montreal group has recently derived family such EoSs based on nuclear energy-density functional theory with generalized Skyrme effective forces, fitted to available mass data. At time, these forces were constrained reproduce microscopic calculations homogeneous matter realistic two- three-nucleon forces. Aims. We represent basic characteristics latest EoS...
We present a new Hartree-Fock-Bogoliubov nuclear mass model based on standard forms of Skyrme and pairing functionals, which corresponds to the most accurate we ever achieved within framework energy density functional theory. Our is characterized by deviation ${\ensuremath{\sigma}}_{\mathrm{mod}}=0.500$ MeV with respect essentially all 2353 available data for nuclei neutron proton numbers larger than 8. At same time, underlying yields realistic description infinite homogeneous matter...
Modeling the composition of neutron-star crusts depends strongly on binding energies neutron-rich nuclides near $N=50$ and $N=82$ shell closures. Using a recent development time-of-flight mass spectrometry for on-line purification radioactive ion beams to access more exotic species, we have determined first time $^{82}\mathrm{Zn}$ with ISOLTRAP setup at ISOLDE-CERN facility. With robust model based nuclear energy-density-functional theory, solve general relativistic...
Even though the ``free'' neutrons in inner crust of a neutron star are superfluid, they still strongly coupled to nuclei due nondissipative entrainment effects. These effects have been systematically studied all regions framework band theory solids. Using concepts from solid-state physics, it is shown that density conduction neutrons, i.e., effectively free, can be much smaller than unbound (by an order magnitude some layers) Bragg scattering. results suggest revision interpretation various...
Large pulsar frequency glitches are generally interpreted as sudden transfers of angular momentum between the neutron superfluid permeating inner crust and rest star. Despite absence viscous drag, is strongly coupled to due nondissipative entrainment effects. These effects shown severely limit maximum amount that can possibly be transferred during glitches. In particular, it found observed in Vela require an additional reservoir momentum.
The equation of state and composition the inner crust neutron stars at zero temperature are calculated, using $T$ $=$ 0 version temperature-dependent extended Thomas-Fermi plus Strutinsky integral method, for each a family three functionals based on Skyrme-type forces BSk19, BSk20, BSk21, which characterized by different degrees symmetry-energy stiffness, also SLy4 functional. We solve Tolman-Oppenheimer-Volkoff equations to calculate distribution mass within crust. Qualitatively similar...
We have calculated the zero-temperature properties of outer crust neutron stars for four nuclear-mass models based on Hartree-Fock-Bogoliubov method: three most recent Skyrme-force (HFB-19, HFB-20, and HFB-21) Gogny-force model D1M. While equation state is substantially same models, nuclidic composition varies considerably from one to another. solve Tolman-Oppenheimer-Volkoff equations by integrating inward surface thereby determine abundance each nuclide in a typical star mass...
We construct a new Hartree-Fock-Bogoliubov (HFB) mass model, labeled HFB-18, with generalized Skyrme force. The additional terms that we have introduced into the force are density-dependent generalizations of usual ${t}_{1}$ and ${t}_{2}$ chosen in such way as to avoid high-density ferromagnetic instability neutron stars is general feature conventional forces, particular forces underlying all HFB models developed past. remaining parameters model then fitted essentially available data, an rms...
The theory of the nuclear energy-density functional is used to provide a unified and thermodynamically consistent treatment all regions cold non-accreting neutron stars. In order assess impact our lack complete knowledge density dependence symmetry energy on constitution global structure stars, we employ four different functionals. All them were precision fitted essentially nuclear-mass data with Hartree-Fock-Bogoliubov method two neutron-matter equations state based realistic forces. For...
Extending our earlier work, a new family of three Hartree-Fock-Bogoliubov (HFB) mass models, labeled HFB-30, HFB-31, and HFB-32, is presented, along with their underlying interactions, BSk30, BSk31, BSk32, respectively. The principle feature purely phenomenological pairing term that depends on the density gradient. This enables us to have bulk fitted realistic nuclear-matter calculations in which for first time self-energy corrections are included, while behavior nucleon effective masses...
Aims. In this paper, we study the global properties of neutron stars (NSs), as predicted by Brussels-Montreal equations state (EoSs). These EoSs, which provide a unified description all regions NS, are based on generalised Skyrme functionals BSk19, BSk20, and BSk21 that were simultaneously fitted to almost nuclear mass data constrained reproduce various infinite matter, obtained from microscopic calculations.
Self-consistent mean-field methods based on phenomenological Skyrme effective interactions are known to exhibit spurious spin and spin-isospin instabilities both at zero finite temperatures when applied homogeneous nuclear matter the densities encountered in neutron stars supernova cores. The origin of these is revisited framework energy density functional theory, a simple prescription proposed remove them. stability several parametrizations reexamined.
We calculate the maximum mass of neutron stars for three different equations state (EOS) based on generalized Skyrme functionals that are simultaneously fitted to essentially all 2003 nuclear data (the rms deviation is 0.58 MeV in cases) and one or other pure matter, each determined by a many-body calculation using realistic two- three-body interactions but leading significantly degrees stiffness at high densities prevailing neutron-star interiors. The observation star with 1.97 $\pm$ 0.04...
Non-empirical effective contact pairing forces to be used in self-consistent mean-field calculations are presented. These forces, constructed so as reproduce exactly any given microscopic gaps infinite homogeneous nuclear matter for isospin asymmetry, analytical form. As a by-product, this work provides an solution of the BCS gap equations which could applied describe various many-body systems.
One of the most intringuing questions about neutron stars concerns their maximum mass. The answer is intimately related to properties matter at densities far beyond that found in heavy atomic nuclei. current view on internal constitution and mass, both from theoretical observational studies, are briefly reviewed.
The Brussels-Montreal Skyrme functionals have been successful in describing properties of both finite nuclei and infinite homogeneous nuclear matter. In their latest version, these equipped with two extra density-dependent terms order to reproduce simultaneously ground state matter while avoiding at the same time arising ferromagnetic instabilities. present article, we extend our previous results linear response theory include such zero temperature pure neutron resulting formalism is then...
When applied to a single nucleon, nuclear energy density functionals may yield nonvanishing internal thus implying that the nucleon is interacting with itself. It shown how avoid this unphysical feature for semilocal phenomenological containing all possible bilinear combinations of local densities and currents up second order in derivatives. The method outlined Rapid Communication could be easily extended higher-order terms, serve as guide constraining time-odd part functional.
An approach to the equation of state for inner crust neutron stars based on Skyrme-type forces is presented. Working within Wigner-Seitz picture, energy calculated by TETF (temperature-dependent extended Thomas-Fermi) method, with proton shell corrections added self-consistently Strutinsky-integral method. Using a Skyrme force that has been fitted both matter and essentially all nuclear mass data, we find strong effects: numbers $Z=50,40$, 20 are only values possible in crust, assuming...
We study the low-energy collective excitations of neutron star inner crust, where a superfluid coexists with Coulomb lattice nuclei. The dispersion relation modes is calculated systematically from microscopic theory including band structure effects. These effects are shown to lead strong mixing between Bogoliubov-Anderson bosons and longitudinal crystal phonons. In addition, speed transverse shear mode greatly reduced as large fraction neutrons entrained by Not only does much smaller...