Abstract
By solving the equations of ideal MHD the interaction of an isothermal coronal plasma with a dipole-like magnetic field is studied. We vary the coronal temperature and the magnetic field strength to investigate how the plasma and the magnetic field interact to determine the structure of the large scale solar corona. When our numerical calculations are initiated with an isothermal solar wind in a dipole magnetic field, the equations may be integrated to a steady state. Open and closed regions are formed. In the open regions the atmosphere expands into a super-sonic wind, and in the closed regions the plasma is in hydrostatic equilibrium. We find that the magnetic field configuration in the outer corona is largely determined by the equatorial current sheet.
| Original language | English |
|---|---|
| Title of host publication | Solar Wind Ten |
| Subtitle of host publication | Proceedings of the 10th International Solar Wind Conference |
| Editors | Marco Velli, Roberto Bruno, Francesco Malara |
| Publisher | American Institute of Physics Inc. |
| Pages | 331-334 |
| Number of pages | 4 |
| ISBN (Electronic) | 0735401489 |
| DOIs | |
| State | Published - Sep 2 2003 |
| Externally published | Yes |
| Event | 10th International Solar Wind Conference - Pisa, Italy Duration: Jun 17 2002 → Jun 21 2002 |
Publication series
| Name | AIP Conference Proceedings |
|---|---|
| Volume | 679 |
| ISSN (Print) | 0094-243X |
| ISSN (Electronic) | 1551-7616 |
Conference
| Conference | 10th International Solar Wind Conference |
|---|---|
| Country/Territory | Italy |
| City | Pisa |
| Period | 06/17/02 → 06/21/02 |
Bibliographical note
Publisher Copyright:© 2003 American Institute of Physics.