Solving the Schrodinger Poisson System using the coordinate Adaptive Moving Mesh method
arXiv:2203.10234 · doi:10.1103/PhysRevD.105.083521
Abstract
In this paper, we implement the Adaptive Moving Mesh method (AMM) to the solution of initial value problems involving the Schrödinger equation, and more specifically the Schrödinger-Poisson system of equations. This method is based on the solution of the problem on a discrete domain, whose resolution is coordinate and time-dependent, and allows to dynamically assign numerical resolution in terms of desired refinement criteria. We apply the method to solve various test problems involving stationary solutions of the SP system, and toy scenarios related to the disruption of subhalo s made of ultralight bosonic dark matter traveling on top of host galaxies.
arXiv comment12 Figures. Published in Physical Review D 105, (2022)8, 083521
References in corpus (44)
- Cosmological Hydrodynamics with Adaptive Mesh Refinement: a new high resolution code called RAMSES
- Cold and Fuzzy Dark Matter
- Ultralight scalars as cosmological dark matter
- Cosmic Structure as the Quantum Interference of a Coherent Dark Wave
- Understanding the Core-Halo Relation of Quantum Wave Dark Matter, DM, from 3D Simulations
- A New Cosmological Model of Quintessence and Dark Matter
- Calibration of Moving Puncture Simulations
- Wave Dark Matter
- Galaxy Formation with BECDM: I. Turbulence and relaxation of idealised haloes
- Simulations of solitonic core mergers in ultra-light axion dark matter cosmologies
- Formation and structure of ultralight bosonic dark matter halos
- Evolution of the Schrödinger--Newton system for a self--gravitating scalar field
- A Review on the Scalar Field/ Bose-Einstein Condensate Dark Matter Model
- Gravitational cooling of self-gravitating Bose-Condensates
- Quintessence and Scalar Dark Matter in the Universe
- Angular Momentum and Vortex Formation in Bose-Einstein-Condensed Cold Dark Matter Haloes
- Scalar Field as Dark Matter in the Universe
- First star-forming structures in fuzzy cosmic filaments
- On the Schrodinger-Poisson--Vlasov-Poisson correspondence
- Galaxy Formation with BECDM -- II. Cosmic Filaments and First Galaxies
- AxioNyx: Simulating Mixed Fuzzy and Cold Dark Matter
- Cosmological constraints on quintessential halos
- Scalar Field Dark Matter: non-spherical collapse and late time behavior
- Tidal disruption of fuzzy dark matter subhalo cores
- Scalar Field Dark Matter: head-on interaction between two structures
- Bosonic gas as a Galactic Dark Matter Halo
- Numerical and Perturbative Computations of the Fuzzy Dark Matter Model
- Brief History of Ultra-light Scalar Dark Matter Models
- PyUltraLight: A Pseudo-Spectral Solver for Ultralight Dark Matter Dynamics
- Gravitational waves from black hole collisions via an eclectic approach
- Vortices and waves in light dark matter
- Construction of Wave Dark Matter Halos: Numerical Algorithm and Analytical Constraints
- Rotation curves of rotating galactic BEC dark matter halos
- Ultra-Light Axion Dark Matter and its impacts on dark halo structure in -body simulation
- Cosmological structure formation in scalar field dark matter with repulsive self-interaction: The Incredible Shrinking Jeans Mass
- Stable vortex in Bose-Einstein condensate dark matter
- Halo Abundance and Assembly History with Extreme-Axion Wave Dark Matter at
- Head-on collision of multi-state ultralight BEC dark matter configurations
- Oscillation modes of ultralight BEC dark matter cores
- Angular Momentum and the Absence of Vortices in the Cores of Fuzzy Dark Matter Haloes
- Energy Balance of a Bose Gas in Curved Spacetime
- Relaxation of structures resulting from head-on mergers of ultralight bosonic dark matter cores
- Merger of galactic cores made of ultralight bosonic dark matter
- Numerical cosmology on the GPU with Enzo and Ramses