Numerical Simulation Of Solar Flare Process

Solar flare is a strong eruptive phenomenon occurring in the solar atmosphere,which releases a large amount of energy within a few minutes.This phenomenon of solar activity has a huge impact on the earth's atmosphere and human life.For flares,current research methods focus on observational studies and numerical simulation studies,the solar activity phenomenon is studied by solving the magnetohydrodynamics equations,but it is very difficult to directly calculate the analytical solution.In this paper,the finite difference method is adopted to solve the equations of magnetohydrodynamics,and the numerical solution is performed by CANS code.The numerical simulation is used to study the effect of solar flare on atmospheric heating,and the process of plasma movement and heating by flare through magnetic reconnection.The main contents are as follows:First,we briefly describe the basic knowledge of flare,coronal mass ejection and magnetic reconnection,and introduce the research background,significance and research progress of flare numerical simulation in detail.Secondly,we simulated the heating and dynamics evolution process of the flare.The one-dimensional numerical simulation is carried out by the modified Lax-Wendroff different method and the Roe scheme.In our model,the length of the are loop,the moment of the beginning of the heating,and the duration of the heating are derived directly from the observations.The cross section is a function of variation with height,the resolution of the transition zone,and the symmetric heating function are modified to make the simulation results closer to the observed phenomenon.The evolution diagram of flare heating is analyzed,and the numerical simulation results can reasonably describe the physical characteristics of flare heating and evolution,and show the formation and development of flare heating,evaporation and condensation of chromosphere.Then,we simulated the magnetic reconnection process in the flare.Two-dimensional numerical simulation was performed by using the modified Lax-Wendroff differential method.Taking the observation as the initial parameter in the simulation,considering the gravity term,and refining the mesh distribution,the evolution diagram of the numerical simulation is obtained.It can be seen from the simulation results that there is an obvious Y-type magnetic current sheet above the magnetic arch during the beginning of the flare energy release.When the current sheet becomes thin and long,an Y-type magnetic current sheet is formed,and a magnetic reconnection phenomenon occurs.As the plasma temperature at the top of the flare increases,a bright soft X-ray ring is formed at the top of the ring,which is in agreement with the observed phenomenon.Finally,we summarized the full text,detailing the innovations?prospects and shortcomings of this paper.