Extended MHD modeling of the steady solar corona and the solar wind
arXiv:1807.00417 · doi:10.1007/s41116-018-0014-4
Abstract
The history and present state of large-scale magnetohydrodynamic (MHD) modeling of the solar corona and the solar wind with steady or quasi-steady coronal physics is reviewed. We put the evolution of ideas leading to the recognition of the existence of an expanding solar atmosphere into historical context. The development and main features of the first generation of global corona and solar wind models are described in detail. This historical perspective is also applied to the present suite of global corona and solar wind models. We discuss the evolution of new ideas and their implementation into numerical simulation codes. We point out the scientific and computational challenges facing these models and discuss the ways various groups tried to overcome these challenges. Next, we discuss the latest, state-of-the art models and point to the expected next steps in modeling the corona and the interplanetary medium.
arXiv commentAccepted for publication, Living Reviews in Solar Physics, 2018
References in corpus (32)
- Alfven Wave Solar Model (AWSoM): Coronal Heating
- Making the corona and the fast solar wind: a self-consistent simulation for the low-frequency Alfven waves from photosphere to 0.3AU
- Alfven Waves and Turbulence in the Solar Atmosphere and Solar Wind
- A turbulence-driven model for heating and acceleration of the fast wind in coronal holes
- Incorporating Kinetic Physics into a Two-Fluid Solar-Wind Model with Temperature Anisotropy and Low-Frequency Alfven-Wave Turbulence
- Empirical Constraints on Proton and Electron Heating in the Fast Solar Wind
- Coronal heating distribution due to low-frequency wave-driven turbulence
- MHD Waves and Coronal Heating: Unifying Empirical and MHD Turbulence Models
- Sun-to-Earth MHD Simulation of the 14 July 2000 "Bastille Day" Eruption
- Connecting the Sun and the Solar Wind: The First 2.5 Dimensional Self-consistent MHD Simulation under the Alfvén Wave Scenario
- Validating a Time-Dependent Wave-Turbulence-Driven Model of the Solar Wind
- A Global Wave-Driven MHD Solar Model with a Unified Treatment of Open and Closed Magnetic Field Topologies
- The Orientation of the Local Interstellar Magnetic Field
- Towards a Realistic, Data-Driven Thermodynamic MHD Model of the Global Solar Corona
- Three-dimensional Features of the Outer Heliosphere Due to Coupling between the Interstellar and Heliospheric Magnetic Field. V. The Bow Wave, Heliospheric Boundary Layer, Instabilities, and Magnetic Reconnection
- Verification of high-speed solar wind stream forecasts using operational solar wind models
- Forecasting Solar Wind Speeds
- Chromosphere to 1 AU Simulation of the 2011 March 7th Event: A Comprehensive Study of Coronal Mass Ejection Propagation
- 2010 August 1-2 sympathetic eruptions: I. Magnetic topology of the source-surface background field
- Comparative Study of MHD Modeling of the Background Solar Wind
- Can the Solar Wind be Driven by Magnetic Reconnection in the Sun's Magnetic Carpet?
- Stochastic Heating, Differential Flow, and the Alpha-to-Proton Temperature Ratio in the Solar Wind
- May 12 1997 Cme Event: I. a Simplified Model of the Pre-Eruptive Magnetic Structure
- Interchange reconnection in a turbulent Corona
- Coronal Heating and Acceleration of the High/Low-Speed Solar Wind by Fast/Slow MHD Shock Trains
- Probing the Edge of the Solar System: Formation of an Unstable Jet-Sheet
- Application of a Solar Wind Model Driven by Turbulence Dissipation to a 2D Magnetic Field Configuration
- Connecting the Sun's High-Resolution Magnetic Carpet to the Turbulent Heliosphere
- Modeling the Solar Wind at the Ulysses, Voyager, and New Horizons Spacecraft
- On the Heating of the Solar Corona and the Acceleration of the Low-Speed Solar Wind by Acoustic Waves Generated in Corona
- Toward Quantitative Model for Simulation and Forecast of Solar Energetic Particles Production during Gradual Events - I: Magnetohydrodynamic Background Coupled to the SEP Model
- Global Asymmetry of the Heliosphere
Cited by in corpus (42)
- Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation
- The Properties of the Solar Corona and Its Connection to the Solar Wind
- What Sustained Multi-Disciplinary Research Can Achieve: The Space Weather Modeling Framework
- The evolution of the solar wind
- Magnetic fields in heavy ion collisions: flow and charge transport
- Morphology of Hydrodynamic Winds: A Study of Planetary Winds in Stellar Environments
- Coronal response to magnetically-suppressed CME events in M-dwarf stars
- Defining the Middle Corona
- Hinode/EIS measurements of active region magnetic fields
- Predictions for the First Parker Solar Probe Encounter
- Simulating the Space Weather in the AU Mic System: Stellar Winds and Extreme Coronal Mass Ejections
- Tuning the Exo-Space Weather Radio for Stellar Coronal Mass Ejections
- Contextual Predictions for Parker Solar Probe I: Critical Surfaces and Regions
- An Extended and Fragmented Alfvén Zone in the Young Solar Wind
- Assessing the Influence of Input Magnetic Maps on Global Modeling of the Solar Wind and CME-driven Shock in the 2013 April 11 Event
- Propulsion of Spacecrafts to Relativistic Speeds Using Natural Astrophysical Sources
- An Earth-like stellar wind environment for Proxima Centauri c
- The winds of young Solar-type stars in the Hyades
- Lambda And: A post-main sequence wind from a solar-mass star
- Coronal mass ejections and type II radio emission variability during a magnetic cycle on the solar-type star Eridani
- SynthIA: A Synthetic Inversion Approximation for the Stokes Vector Fusing SDO and Hinode into a Virtual Observatory
- Breezing through the space environment of Barnard's Star b
- Global Coronal Equilibria with Solar Wind Outflow
- Numerical quantification of the wind properties of cool main sequence stars
- Electric sails are potentially more effective than light sails near most stars
- Electron Heat Flux in the Solar Wind: Generalized Approaches to Fluid Transport with a Variety of Skewed Velocity Distributions
- HOW-MHD: A High-Order WENO-Based Magnetohydrodynamic Code with a High-Order Constrained Transport Algorithm for Astrophysical Applications
- Stellar Energetic Particle Transport in the Turbulent and CME-disrupted Stellar Wind of AU~Microscopii
- Stream-Aligned Magnetohydrodynamics for Solar Wind Simulations
- Physics-Based Simulation of the 2013 April 11 Solar Energetic Particle Event
- SIP-IFVM: Efficient time-accurate magnetohydrodynamic model of the corona and coronal mass ejections
- Evidence of Time-Dependent Diffusive Shock Acceleration in the 2022 September 5 Solar Energetic Particle Event
- The effect of turbulence on the angular momentum of the solar wind
- Space weather: the solar perspective -- an update to Schwenn (2006)
- Ensemble Modeling of the Solar Wind Flow with Boundary Conditions Governed by Synchronic Photospheric Magnetograms. I. Multi-point Validation in the Inner Heliosphere
- NIRwave: A wave-turbulence-driven solar wind model constrained by PSP observations
- Three-dimensional, Time-dependent MHD Simulation of Disk-Magnetosphere-Stellar Wind Interaction in a T Tauri, Protoplanetary System
- Solar Wind Penetration into Dusty Magnetospheres creates Electrostatic Waves and Structures
- Optimal Landau-type closure parameters for two-fluid simulations of plasma turbulence at kinetic scales
- The winds of young Solar-type stars in Coma Berenices and Hercules-Lyra
- Coronal Mass Ejections and Exoplanets: A Numerical Perspective
- (Simulating) Coronal Mass Ejections in Active Stars