Abstract
In this paper, the spacetime conservation element and solution element (CESE) method is applied to three-dimensional magnetohydrodynamics (MHD) equations in Cartesian coordinates for solar wind plasma, with the purpose of modeling the steady state solar atmospheric study. To illustrate this newly developed scheme we have studied two examples: (1) two-dimensional coronal dynamical structure with multipole magnetic fields and (2) three-dimensional coronal dynamical structure, using measured solar surface magnetic fields and the empirical values of the plasma properties on the solar surface as the initial conditions for the set of MHD equations and then the relaxation method to achieve a quasi-steady state. From these examples we have shown that the newly developed modified spacetime CESE scheme possesses the ability to model the Sun-Earth environment and other astrophysical flows.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
