A5034546383- Pulsars and Gravitational Waves Research
- Gamma-ray bursts and supernovae
- Cosmology and Gravitation Theories
- High-pressure geophysics and materials
- Astrophysical Phenomena and Observations
- Geophysics and Gravity Measurements
- Magnetic confinement fusion research
- Atomic and Subatomic Physics Research
- Black Holes and Theoretical Physics
- Cold Atom Physics and Bose-Einstein Condensates
- Dark Matter and Cosmic Phenomena
- Advanced Frequency and Time Standards
- Radio Astronomy Observations and Technology
- Seismic Waves and Analysis
- Geophysics and Sensor Technology
- Mechanical and Optical Resonators
- Radiology practices and education
- Fluid Dynamics and Turbulent Flows
- Economic, financial, and policy analysis
- High-Energy Particle Collisions Research
- Quantum, superfluid, helium dynamics
- earthquake and tectonic studies
- Superconducting Materials and Applications
- Statistical and numerical algorithms
- Meteorological Phenomena and Simulations
Universitat de València
2021-2025
Université Paris Cité
2023
Laboratoire AstroParticule et Cosmologie
2023
Centre National de la Recherche Scientifique
2023
Istituto Nazionale di Fisica Nucleare, Sezione di Roma I
2019
Sapienza University of Rome
2019
We study novel solitonic solutions to Einstein-Klein-Gordon theory in the presence of a periodic scalar potential arising models axion-like particles.The depends on two parameters: mass field m and decay constant f ; standard case QCD axion is recovered when ∝ 1/f .When → ∞ reduce "mini" boson stars supported by massive free field.As energy scale self-interactions decreases we unveil several features solution: new stability branches emerge at high density, giving rise very compact, radially...
Explaining gravitational-wave (GW) observations of binary neutron star (BNS) mergers requires an understanding matter beyond nuclear saturation density. Our current knowledge the properties high-density relies on electromagnetic and GW observations, physics experiments, general relativistic numerical simulations. Using a phenomenological nonconvex equation state (EoS) we conduct suite numerical-relativity simulations BNS identify observable imprints spectra remnant. Nonconvex regions may be...
Explaining gravitational-wave (GW) observations of binary neutron star (BNS) mergers requires an understanding matter beyond nuclear saturation density. Our current knowledge the properties high-density relies on electromagnetic and GW observations, physics experiments, general relativistic numerical simulations. In this paper we perform numerical-relativity simulations BNS subject to nonconvex dynamics, allowing for appearance expansive shock waves compressive rarefactions. Using a...
We construct spherically symmetric static solutions of the Einstein-Klein-Gordon-Euler system involving a complex scalar field governed by periodic potential that emerges in models axionlike particles and fermionic matter modeled perfect fluid with polytropic equation state. Such describe gravitationally bound composites fermions axions, which we dub fermion-axion stars. Sequences pure axion stars existence domain may show presence multiple stable branches depending on value decay constant...
We investigate the effects ultralight bosonic field dark matter may have on dynamics of unstable differentially-rotating neutron stars prone to bar-mode instability. To this aim we perform numerical simulations in general relativity rotating accreting an initial spherically symmetric cloud, solving Einstein-(complex, massive) Klein-Gordon-Euler and Einstein-(complex) Proca-Euler systems. find that presence can critically modify development instability stars, depending total mass boson...
We explore the prospects for identifying differences in simulated gravitational-wave signals of binary neutron star (BNS) mergers associated with way thermal effects are incorporated numerical-relativity modelling. consider a hybrid approach which equation state (EoS) comprises cold, zero temperature, piecewise-polytropic part and described by an ideal gas, tabulated based on self-consistent, microphysical, finite-temperature EoS. use time-domain waveforms corresponding to BNS merger...
Explaining gravitational-wave (GW) observations of binary neutron star (BNS) mergers requires an understanding matter beyond nuclear saturation density. Our current knowledge the properties high-density relies on electromagnetic and GW observations, physics experiments, general relativistic numerical simulations. In this paper we perform numerical-relativity simulations BNS subject to non-convex dynamics, allowing for appearance expansive shock waves compressive rarefactions. Using a...
We assess the impact of accurate, self-consistent modelling thermal effects in neutron-star merger remnants context third-generation gravitational-wave detectors. This is done through usage, Bayesian model selection experiments, numerical-relativity simulations binary neutron star (BNS) mergers modelled through: a) nuclear, finite-temperature (or ``tabulated'') equations state (EoSs), and b) their simplifed piecewise ``hybrid'') representation. These cover four different EoSs, namely SLy4,...
We construct spherically-symmetric static solutions of the Einstein-Klein-Gordon-Euler system involving a complex scalar field governed by periodic potential which emerges in models axion-like particles, and fermionic matter modeled perfect fluid with polytropic equation state. Such describe gravitationally bound composites fermions axions we dub as fermion-axion stars. Sequences pure axion-stars existence domain may show presence multiple stable branches depending on value decay constant...