Integrating physics-based coronal heating and solar wind acceleration in a global MHD model

2013 ◽  
Author(s):  
Roberto Lionello ◽  
Marco Velli ◽  
Jon A. Linker ◽  
Zoran Mikić
Keyword(s):  
Solar Wind ◽  
Coronal Heating ◽  
Solar Wind Acceleration ◽  
Mhd Model

scholarly journals A STEADY-STATE PICTURE OF SOLAR WIND ACCELERATION AND CHARGE STATE COMPOSITION DERIVED FROM A GLOBAL WAVE-DRIVEN MHD MODEL

2015 ◽  
Vol 806 (1) ◽  
pp. 55 ◽  
Author(s):  
R. Oran ◽  
E. Landi ◽  
B. van der Holst ◽  
S. T. Lepri ◽  
A. M. Vásquez ◽  
...  
Keyword(s):  
Solar Wind ◽  
Steady State ◽  
Charge State ◽  
Solar Wind Acceleration ◽  
Mhd Model ◽  
State Composition

scholarly journals Numerical Study of Divergence Cleaning and Coronal Heating/Acceleration Methods in the 3D COIN-TVD MHD Model

2021 ◽  
Vol 9 ◽  
Author(s):  
Chang Liu ◽  
Fang Shen ◽  
Yousheng Liu ◽  
Man Zhang ◽  
Xiaojing Liu
Keyword(s):  
Solar Wind ◽  
Numerical Study ◽  
Three Dimensional ◽  
Coronal Heating ◽  
Solar Wind Structure ◽  
Wind Simulation ◽  
Simulation Results ◽  
Mhd Model ◽  
Cleaning Methods ◽  
Powell Method

In the solar coronal numerical simulation, the coronal heating/acceleration and the magnetic divergence cleaning techniques are very important. The coronal–interplanetary total variation diminishing (COIN-TVD) magnetohydrodynamic (MHD) model is developed in recent years that can effectively realize the coronal–interplanetary three-dimensional (3D) solar wind simulation. In this study, we focus on the 3D coronal solar wind simulation by using the COIN-TVD MHD model. In order to simulate the heating and acceleration of solar wind in the coronal region, the volume heating term in the model is improved efficiently. Then, the influence of the different methods to reduce the ∇⋅B constraint error on the coronal solar wind structure is discussed. Here, we choose Carrington Rotation (CR) 2199 as a study case and try to make a comparison of the simulation results among the different magnetic divergence cleaning methods, including the diffusive method, the Powell method, and the composite diffusive/Powell method, by using the 3D COIN-TVD MHD model. Our simulation results show that with the different magnetic divergence cleaning methods, the ∇⋅B error can be reduced in different levels during the solar wind simulation. Among the three divergence cleaning methods we used, the composite diffusive/Powell method can maintain the divergence cleaning constraint better to a certain extent, and the relative magnetic field divergence error can be controlled in the order of 10−9. Although these numerical simulations are performed for the background solar corona, these methods are also suitable for the simulation of CME initiation and propagation.

scholarly journals Understanding coronal heating and solar wind acceleration: Case for in situ near-Sun measurements

2007 ◽  
Vol 45 (1) ◽  
Author(s):  
D. J. McComas ◽  
M. Velli ◽  
W. S. Lewis ◽  
L. W. Acton ◽  
M. Balat-Pichelin ◽  
...  
Keyword(s):  
Solar Wind ◽  
Coronal Heating ◽  
Solar Wind Acceleration

MULTI-SHELL MAGNETIC TWISTERS AS A NEW MECHANISM FOR CORONAL HEATING AND SOLAR WIND ACCELERATION

2015 ◽  
Vol 808 (1) ◽  
pp. 5 ◽  
Author(s):  
K. Murawski ◽  
A. K. Srivastava ◽  
Z. E. Musielak ◽  
B. N. Dwivedi
Keyword(s):  
Solar Wind ◽  
Coronal Heating ◽  
Solar Wind Acceleration

scholarly journals Coronal Heating and the Solar Wind Acceleration

2001 ◽  
Vol 203 ◽  
pp. 495-497 ◽  
Author(s):  
T. Hirayama
Keyword(s):  
Solar Wind ◽  
Electric Field ◽  
Dissipation Rate ◽  
Electron Beams ◽  
Coronal Heating ◽  
Thermal Electron ◽  
Charge Imbalance ◽  
Solar Wind Acceleration

We propose a coronal heating theory based on the magnetic twisting, which inevitably produces charge imbalance. The resulting electric field creates supra-thermal electron beams. Beams are then thermalized by classical collisions. The dissipation rate is enough to heat the corona and to accelerate the solar wind.

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