Abstract A three-dimensional, time-dependent magnetohydrodynamic (MHD) model is presented for the study of coronal dynamics. The model, written in spherical coordinates, extends from the solar surface (1R s, where 1R s = 6.95 × 105 km) to 15 R s. This model was developed with two major issues in mind, namely for interpretation of various steady state and evolutionary dynamical structures in the corona. In order to achieve these objectives we have employed two different numerical techniques to seek solutions for these two different, but related, problems; steady state structures and evolutionary structures. These two numerical techniques are: (i) relaxation technique for steady state structures; and (ii) FICE (Full-Implicit-Continuous-Eulerian) technique for evolutionary structures. To illustrate this model, we present numerical results for examples of both the steady state and evolutionary structure of the corona. These results show the additional physical features which cannot be shown by a two-dimensional model. Finally, on the basis of the exploratory calculation, we outline some interesting physical features which can be considered for the observing programs of future space missions such as SOHO, OSL, CORONAS, etc.


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    Titel :

    Numerical simulation of extended corona


    Beteiligte:
    Wu, S.T. (Autor:in) / Wang, Ai-Hwa (Autor:in)

    Erschienen in:

    Advances in Space Research ; 11 , 1 ; 187-195


    Erscheinungsdatum :

    1991-01-01


    Format / Umfang :

    9 pages




    Medientyp :

    Aufsatz (Zeitschrift)


    Format :

    Elektronische Ressource


    Sprache :

    Englisch



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