A three-dimensional, time-dependent MHD model is presented for the study of coronal dynamics. The model, written in spherical coordinates, extends from the solar surface and 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, two different numerical techniques are used to seek solutions for these two different, but related, problems; steady state structures and evolutionary structures. These two numerical techniques are: (1) relaxation technique for steady state structures; and (2) FICE (Full-Implicit-Continuous-Eulerian) technique for evolutionary structures. To illustrate this model, numerical results are given for examples of both the steady state and evolutionary structure of the corona which show the additional physical features which cannot be shown by a two-dimensional model.
Numerical simulation of extended corona
Advances in Space Research ; 11 , 1 19
1991-01-01
Sonstige
Keine Angabe
Englisch
Numerical simulation of extended corona
Elsevier | 1991
|Diagnostic methods for the extended corona
Elsevier | 1991
|UV observations of the extended corona
Elsevier | 1991
|Measuring Electron Temperature in the Extended Corona
British Library Online Contents | 1992
|UV observational techniques for the extended solar corona
Elsevier | 1991
|