MHD Modeling of the Solar Corona
Abstract
The structure of the solar corona is determined to a large extent by the magnetic field. Unfortunately, it is not possible to measure the magnetic field in the corona (in general). To maximize the interpretation of solar observations it is therefore necessary to use theoretical models. By using a three-dimensional MHD model to describe the self-consistent interaction of magnetic, plasma, and gravity forces, including the effect of the solar wind, it is possible to determine the large-scale structure of the magnetic field in the corona and inner heliosphere, as well as the distribution of the solar wind velocity, plasma density, and temperature. The model can provide quantitative outputs that can be tested directly against observations, including coronagraph images, in situ solar wind and magnetic field measurements, heliospheric current sheet crossings, interplanetary scintillation measurements, and emissions in various radiation lines. The principal input to the model is the observed photospheric magnetic field. Comparisons between the model and eclipse observations, coronagraph observations, SOHO data, and Ulysses and WIND interplanetary plasma measurements will be presented. Research sponsored by NASA and NSF. Computations performed at NERSC and SDSC.
- Publication:
-
APS Division of Plasma Physics Meeting Abstracts
- Pub Date:
- November 1998
- Bibcode:
- 1998APS..DPPD2I204M