| Issue |
A&A
Volume 371, Number 1, May III 2001
|
|
|---|---|---|
| Page(s) | 328 - 332 | |
| Section | Planets and planetary systems | |
| DOI | https://doi.org/10.1051/0004-6361:20010315 | |
| Published online | 15 May 2001 | |
Solar prominence magnetic configurations derived numerically from convection
Department of Mathematics, Tidewater Community College, Virginia Beach, VA 23456, USA
Received:
19
January
2001
Accepted:
28
February
2001
The solar convection zone may be a mechanism for generating the magnetic fields in the corona that create and thermally insulate quiescent prominences. This connection is examined here by numerically solving a diffusion equation with convection (below the photosphere) matched to Laplace's equation (modeling the current free corona above the photosphere). The types of fields formed resemble both Kippenhahn-Schlüter and Kuperus-Raadu configurations with feet that drop into supergranule boundaries.
Key words: supergranulation / convection / prominences
© ESO, 2001
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.