Full compressible 3D magnetohydrodynamic simulation of solar wind

Abstract

Identifying the heating mechanisms of the solar corona and the driving mechanisms of solar wind are key challenges in understanding solar physics. A full three-dimensional compressible magnetohydrodynamic (MHD) simulation was conducted to distinguish between the heating mechanisms in the fast solar wind above the open field region. Our simulation describes the evolution of the Alfvénic waves, which includes the compressible effects from the photosphere to the heliospheric distance $s$ of 27 solar radii ($R_{\odot }$). The hot corona and fast solar wind were reproduced simultaneously due to the dissipation of the Alfvén waves. The inclusion of the transition region and lower atmosphere enabled us to derive the solar mass loss rate for the first time by performing a full three-dimensional compressible MHD simulation. The Alfvén turbulence was determined to be the dominant heating mechanism in the solar wind acceleration region ($s>1.3R_{\odot }$), as suggested by previous solar wind models. In addition, shock formation and phase mixing are important below the lower transition region ($s<1.03R_{\odot }$) as well.

arXiv comment9 pages, 7 figures, accepted for publication in MNRAS

References in corpus (38)

• On Solving the Coronal Heating Problem
• Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence
• New Mass Loss Measurements from Astrospheric Lyman-alpha Absorption
• On the Generation, Propagation, and Reflection of Alfven Waves from the Solar Photosphere to the Distant Heliosphere
• Heating of the Solar Chromosphere and Corona by Alfven Wave Turbulence
• Coronal Holes
• Testing a Predictive Theoretical Model for the Mass Loss Rates of Cool Stars
• Making the corona and the fast solar wind: a self-consistent simulation for the low-frequency Alfven waves from photosphere to 0.3AU
• Efficient, High Accuracy ADER-WENO Schemes for Hydrodynamics and Divergence-Free Magnetohydrodynamics
• 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
• Magnetic Landscape of Sun's Polar Region
• Incorporating Kinetic Physics into a Two-Fluid Solar-Wind Model with Temperature Anisotropy and Low-Frequency Alfven-Wave Turbulence
• Coronal heating distribution due to low-frequency wave-driven turbulence
• Divergence-Free Reconstruction of Magnetic Fields and WENO Schemes for Magnetohydrodynamics
• Solar Winds Driven by Nonlinear Low-Frequency Alfven Waves from the Photosphere : Parametric Study for Fast/Slow Winds and Disappearance of Solar Winds
• Nonlinear propagation of Alfven waves driven by observed photospheric motions: Application to the coronal heating and spicule formation
• Connecting the Sun and the Solar Wind: The First 2.5 Dimensional Self-consistent MHD Simulation under the Alfvén Wave Scenario
• Alfven Wave Collisions, The Fundamental Building Block of Plasma Turbulence I: Asymptotic Solution
• Heating and Acceleration of the Fast Solar Wind by Alfvén Wave Turbulence
• Polar Field Reversal Observations with Hinode
• Forecasting Solar Wind Speeds
• Connecting the Sun and the Solar Wind: The Self-consistent Transition of Heating Mechanisms
• Is the Polar Region Different from the Quiet Region of the Sun?
• Three-dimensional simulation of the fast solar wind driven by compressible magnetohydrodynamic turbulence
• Reflection-driven MHD turbulence in the solar atmosphere and solar wind
• Dynamics of the Solar Magnetic Network: Two-dimensional MHD Simulations
• Dynamics of the solar magnetic bright points derived from their horizontal motions
• Saturation of Stellar Winds from Young Suns
• A self-consistent model of the coronal heating and solar wind acceleration including compressible and incompressible heating processes
• Temporal power spectra of the horizontal velocity of the solar photosphere
• Spectrum of weak magnetohydrodynamic turbulence
• Generation of Magnetohydrodynamic Waves in Low Solar Atmospheric Flux Tubes by Photospheric Motions
• Coronal heating in coupled photosphere-chromosphere-coronal systems: turbulence and leakage
• Alfvén-wave driven magnetic rotator winds from low-mass stars I: rotation dependences of magnetic braking and mass-loss rate
• Anisotropic magnetohydrodynamic turbulence driven by parametric decay instability: the onset of phase mixing and Alfvén wave turbulence
• Competition between shock and turbulent heating in coronal loop system
• Average radial structures of gas convection in the solar granulation

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• Role of Longitudinal Waves in Alfvén-wave-driven Solar Wind
• Nonlinear Alfvén Wave Model of Stellar Coronae and Winds from the Sun to M dwarfs
• The Effect of the Chromospheric Temperature on Coronal Heating
• Coronal Properties of Low-mass Population III Stars and the Radiative Feedback in the Early Universe
• Stellar X-rays and magnetic activity in 3D MHD coronal models
• What Determines the Brightness of the Magnetically Open Solar Corona?: Insights from Three-dimensional Radiative Magnetohydrodynamic Simulations and Observations