A5052915143- Stellar, planetary, and galactic studies
- Astrophysics and Star Formation Studies
- Galaxies: Formation, Evolution, Phenomena
- Solar and Space Plasma Dynamics
- Computational Fluid Dynamics and Aerodynamics
- Astronomy and Astrophysical Research
- Astro and Planetary Science
- Topological Materials and Phenomena
- Scientific Research and Discoveries
- Astrophysics and Cosmic Phenomena
- Advanced Numerical Methods in Computational Mathematics
- Magnetic and transport properties of perovskites and related materials
- Cosmology and Gravitation Theories
- Electronic and Structural Properties of Oxides
- Meteorological Phenomena and Simulations
- Astrophysical Phenomena and Observations
- Gas Dynamics and Kinetic Theory
- Magnetic properties of thin films
- 3D Surveying and Cultural Heritage
- Computational Physics and Python Applications
- Solar Radiation and Photovoltaics
- Remote Sensing and LiDAR Applications
- Model Reduction and Neural Networks
- Advanced Condensed Matter Physics
- Oceanographic and Atmospheric Processes
University of Exeter
2019-2025
Institut Català de Nanociència i Nanotecnologia
2023
Commissariat à l'Énergie Atomique et aux Énergies Alternatives
2010-2022
Université Grenoble Alpes
2022
CEA Grenoble
2022
Centre National de la Recherche Scientifique
2022
Spintronique et Technologie des Composants
2022
Direction de la Recherche Technologique
2022
Heidelberg University
2017-2019
Heidelberg Institute for Theoretical Studies
2017-2019
The magnetic fields observed in the Milky~Way and nearby galaxies appear to be equipartition with turbulent, thermal, cosmic ray energy densities, hence are expected dynamically important. However, origin of these strong is still unclear, most previous attempts simulate galaxy formation from cosmological initial conditions have ignored them altogether. Here, we analyse predicted by simulations Auriga Project, a set 30 high-resolution zoom Milky~Way-like galaxies, carried out moving-mesh...
Cosmological simulations are an important theoretical pillar for understanding nonlinear structure formation in our Universe and relating it to observations on large scales. In several papers, we introduce MillenniumTNG (MTNG) project that provides a comprehensive set of high-resolution, volume cosmic aiming better understand physical processes scales help interpreting upcoming large-scale galaxy surveys. We here focus the full physics box MTNG740 computes $(740\,\mathrm{Mpc})^3$ with...
We perform two-dimensional numerical simulations of core convection for zero-age-main-sequence stars covering a mass range from 3 $M_\odot$ to 20 $M_\odot$. The are performed with the fully compressible time-implicit code MUSIC. study efficiency overshooting, which describes ballistic process convective flows crossing boundary, as function stellar and luminosity. also impact artificially increasing luminosity models. cover hundreds thousands turnover timescales. Applying framework extreme...
ABSTRACT Magnetic fields are ubiquitous in the Universe. Recently, cosmological simulations of galaxies have successfully begun to incorporate magnetic and their evolution haloes. However, so far they mostly focused on Milky Way-like galaxies. Here, we analyse a sample high-resolution zoom disc haloes with mass ${M}_\rm {200c}$ from $10^{10}$ $10^{13}\, \rm {M}_\odot$, simulated Auriga galaxy formation model. We show that sufficient numerical resolution field amplification saturation is...
The circumgalactic medium (CGM) is one of the frontiers galaxy formation and intimately connected to via accretion gas on gaseous outflows from galaxy. Here we analyse magnetic field in CGM Milky Way-like galaxies simulated as part \textsc{Auriga} project that constitutes a set high resolution cosmological magnetohydrodynamical zoom simulations. We show before $z=1$ becomes magnetised galactic transport disk into halo. At this time magnetisation closely follows its metal enrichment. then at...
Faraday rotation is one of the most widely used observables to infer strength and configuration magnetic field in ionized gas Milky Way nearby spiral galaxies. Here, we compute synthetic maps at |$z$| = 0 for a set disc galaxies from Auriga high-resolution cosmological simulations, different observer positions within outside galaxy. We find that our simulated hypothetic solar circle broadly consistent with seen Way. The same holds an galaxy observed signal M51. However, also structure...
Our ability to predict the structure and evolution of stars is in part limited by complex, 3D hydrodynamic processes such as convective boundary mixing. Hydrodynamic simulations help us understand dynamics stellar convection boundaries. However, codes used compute are usually tested on extremely simple problems reliability reproducibility their predictions for turbulent flows unclear. We define a test problem involving plane-parallel box, which leads mass entrainment from, internal-wave...
ABSTRACT Here we present a study of radial chemical mixing in non-rotating massive main-sequence stars driven by internal gravity waves (IGWs), based on multidimensional hydrodynamical simulations with the fully compressible code MUSIC. We examine two proposed mechanisms material IGWs that are commonly quoted, relating to thermal diffusion and sub-wavelength shearing. Thermal provides non-restorative effect waves, leaving displaced from its previous equilibrium, while shearing arising within...
We study the dissipative effects of baryon physics on cosmic statistics at small scales using a cosmological simulation (50 Mpc h−1)3 volume universe. The MareNostrum was performed adaptive mesh refinement (AMR) code ramses, and includes most physical ingredients which are part current theory galaxy formation, such as metal-dependent cooling UV heating, subgrid modelling interstellar medium, star formation supernova feedback. reran same initial conditions for dark matter only universe,...
Modern astrophysical simulations aim to accurately model an ever-growing array of physical processes, including the interaction fluids with magnetic fields, under increasingly stringent performance and scalability requirements driven by present-day trends in computing architectures. Discontinuous Galerkin (DG) methods have recently gained some traction astrophysics, because their arbitrarily high order controllable numerical diffusion, combined attractive characteristics for high-performance...
Artificially increasing the luminosity and thermal diffusivity of a model is common tactic adopted in hydrodynamical simulations stellar convection. In this work, we analyse impact these artificial modifications on physical properties interiors specifically internal gravity waves. We perform two-dimensional solar-like stars with MUSIC code. compare three models different enhancement factors to reference model. The results confirm that waves are impacted by diffusivity. find an increase...
Main-sequence intermediate-mass stars present a radiative envelope that supports internal gravity waves (IGWs). Excited at the boundary with convective core, IGWs propagate towards stellar surface and are suspected to impact physical processes such as rotation chemical mixing. Using fully compressible time-implicit code MUSIC, we study in two-dimensional simulations of zero-age-main-sequence 5 solar mass star model up 91\% radius different luminosity diffusivity enhancements. Our results...
We performed two-dimensional, fully compressible, time-implicit simulations of convection in a solar-like model with the MUSIC code. Our main motivation is to explore impact common tactic adopted numerical that use realistic stellar conditions. This artificially increase luminosity and modify thermal diffusivity reference model. work focuses on these modifications convective penetration (or overshooting) at base envelope range enhancement factors for energy input luminosity) confirm...
Spin-orbit effects appearing in topological insulators (TI) and at Rashba interfaces are currently revolutionizing how we can manipulate spins have led to several newly discovered effects, from spin-charge interconversion spin-orbit torques novel magnetoresistance phenomena. In particular, a puzzling has been evidenced as bilinear electric magnetic fields. Here, report the observation of (BMR) strained HgTe, prototypical TI. We show that both amplitude sign this BMR be tuned by controlling...
Cosmological simulations are an important theoretical pillar for understanding nonlinear structure formation in our Universe and relating it to observations on large scales. In several papers, we introduce MillenniumTNG (MTNG) project that provides a comprehensive set of high-resolution, volume cosmic aiming better understand physical processes scales help interpreting upcoming large-scale galaxy surveys. We here focus the full physics box MTNG740 computes $(740\,\mathrm{Mpc})^3$ with...
Hydrodynamical numerical methods that converge with high-order hold particular promise for astrophysical studies, as they can in principle reach prescribed accuracy goals higher computational efficiency than standard second- or third-order approaches. Here we consider the performance and benefits of Discontinuous Galerkin (DG) methods, which offer a particularly straightforward approach to extremely high order. Also, their stencil maps well modern GPU devices, further raising attractiveness...
We investigate the numerical performance of a Discontinuous Galerkin (DG) hydrodynamics implementation when applied to problem driven, isothermal supersonic turbulence. While high-order element-based spectral approach DG is known efficiently produce accurate results for smooth problems (exponential convergence with expansion order), physical discontinuities in solutions, like shocks, prove challenging and may significantly diminish DG's applicability practical astrophysical applications....
As a massive star evolves along the main sequence, its core contracts, leaving behind stable stratification in helium. We simulate 2D convection at three different stages of evolution $5M_{\odot}$ star, with stratifications helium atop core. study propagation internal gravity waves stably-stratified envelope, overshooting length convective plumes above boundary. find that evolved stars hinders radial motions and effectively shields radiative envelope against plume penetration. This prevents...
We compute rotating 1D stellar evolution models that include a modified temperature gradient in convection zones and criterion for convective instability inspired by 3D hydrodynamical simulations performed with the MUSIC code. In those we found properties strongly depend on Solberg–Høiland stability. therefore incorporated this into replacing usual Schwarzschild stability also modifying zones. computed grid of between 0.55 1.2 masses from pre-main sequence to end main order study problem...
A new solver featuring time-space adaptation and error control has been recently introduced to tackle the numerical solution of stiff reaction-diffusion systems. Based on operator splitting, finite volume adaptive multiresolution high order time integrators with specific stability properties for each operator, this strategy yields computational efficiency large multidimensional computations standard architectures such as powerful workstations. However, data structure original implementation,...
Recent hydrodynamical simulations of convection in a solar-like model suggest that penetrative convective flows at the boundary envelope modify thermal background overshooting layer. Based on these results, we implement one-dimensional stellar evolution codes simple prescription to temperature gradient below solar model. This qualitatively reproduces behaviour found simulations, namely local heating and smoothing boundary. We show introducing layer can reduce sound-speed discrepancy usually...
ABSTRACT Stellar convection is a non-local process responsible for the transport of heat and chemical species. It can lead to enhanced mixing through convective overshooting excitation internal gravity waves (IGWs) at boundaries. The relationship between these processes still not well understood requires global hydrodynamic simulations capture important large-scale dynamics. steep stratification in stellar interiors suggests that radial extent such affect dynamics, IGWs stably stratified...
Abstract We investigate the numerical performance of a Discontinuous Galerkin (DG) hydrodynamics implementation when applied to problem driven, isothermal supersonic turbulence. While high-order element-based spectral approach DG is known efficiently produce accurate results for smooth problems (exponential convergence with expansion order), physical discontinuities in solutions, like shocks, prove challenging and may significantly diminish DG’s applicability practical astrophysical...