Preliminary Simulation Of Coronal Acceleration/Heating And Magnetic Field Divergence Controlling In Coronal Numerical Modeling

The corona-interplanetary solar wind three-dimensional numerical simulation is an important method for forecasting space weather.In the corona three-dimensional solar wind numerical simulation,the simulation of the corona acceleration heating and the processing of the magnetic field divergence are the problems that must be solved in the simulation work,in order that the simulation results can be compared with the actual solar wind status is consistent,achieving the purpose of accurate forecasting.In this paper,the COIN-TVD MHD model developed in recent years is used to study the three-dimensional solar wind in the coronal region,simulating Carrington Rotation 2199.According to the characteristics of the high temperature in the corona region and the acceleration of the solar wind in this region,the volume heating term in the model is improved.Discuss the influence of different methods to reduce the error of the magnetic field divergence on the structure of the coronal solar wind.The Powell method,the diffusive method,and the diffusive and Powell method are used to deal with the problem that the magnetic field divergence is not zero,and they are analyzed and compared.The simulation results show that the combination of the diffusive method and the Powell method to process the magnetic field divergence can control the relative magnetic field divergence error within 10^-9.The improved three-dimensional solar wind model of the corona is effective in the process of solar wind acceleration and magnetic field divergence in the corona area.Performance has been improved to a certain extent.